## 2015A&A.submitted - 2.5D global-disk oscillation models of the Be shell star zeta Tauri I. Spectroscopic and polarimetric analysis

C. Escolano, A. C. Carciofi, A. T. Okazaki, T. Rivinius, D. Baade, S. Stefl
Abstract: Context. Various Be stars exhibit intensity variations of the violet and red emission peaks in their HI lines observed in emission. This so-called $V/R$ phenomenon is usually explained by the precession of a one-armed spiral density perturbation in the circumstellar disk. That global-disk oscillation scenario was confirmed, both observationally and theoretically, in the previous series of two papers analyzing the Be shell star {\zeta} Tauri. The vertically averaged (2D) global-disk oscillation model used at the time was able to reproduce the $V/R$ variations observed in H{\alpha}, as well as the spatially resolved interferometric data from AMBER/VLTI. Unfortunately, that model failed to reproduce the $V/R$ phase of Br15 and the amplitude of the polarization variation, suggesting that the inner disk structure predicted by the model was incorrect. Aims. The first aim of the present paper is to quantify the temporal variations of the shell-line characteristics of {\zeta} Tauri. The second aim is to better understand the physics underlying the $V/R$ phenomenon by modeling the shell-line variations together with the $V/R$ and polarimetric variations. The third aim is to test a new 2.5D disk oscillation model, which solves the set of equations that describe the 3D perturbed disk structure but keeps only the equatorial (i.e., 2D) component of the solution. This approximation was adopted to allow comparisons with the previous 2D model, and as a first step toward a future 3D model. Results. The new 2.5D formalism improves the agreement with the observed $V/R$ variations of H{\alpha} and Br15, under the proviso that a large value of the viscosity parameter, {\alpha} = 0.8, be adopted. Nonetheless, it remains challenging for the models to reproduce consistently the amplitude and the average level of the polarization data, whatever formalism is adopted.
Full text: http://arxiv.org/abs/1503.00590v1

## 2015MNRAS...446..274 - A deep catalogue of classical Be stars in the direction of the Perseus Arm: spectral types and interstellar reddenings

R. Raddi, J. E. Drew, D. Steeghs, N. J. Wright, J. J. Drake, G. Barentsen, J. Fabregat, S. E. Sale
Abstract: We present a catalogue of 247 photometrically and spectroscopically confirmed fainter classical Be stars (13 < r < 16) in the direction of the Perseus Arm of the Milky Way (-1 < b < +4, 120 < l < 140). The catalogue consists of 181 IPHAS-selected new classical Be stars, in addition to 66 objects that were studied by Raddi et al. (2013) more closely, and 3 stars identified as classical Be stars in earlier work. This study more than doubles the number known in the region. Photometry spanning 0.6 to 5 micron, spectral types, and interstellar reddenings are given for each object. The spectral types were determined from low-resolution spectra (lambda / Delta-lambda ~ 800-2000), to a precision of 1-3 subtypes. The interstellar reddenings are derived from the (r - i) colour, using a method that corrects for circumstellar disc emission. The colour excesses obtained range from E(B-V) = 0.3 up to 1.6 - a distribution that modestly extends the range reported in the literature for Perseus-Arm open clusters. For around half the sample, the reddenings obtained are compatible with measures of the total sightline Galactic extinction. Many of these are likely to lie well beyond the Perseus Arm.
Full text: http://arxiv.org/abs/1410.1533v1

## 2015JBAA.Accepted - Photometric and spectroscopic observations of the 2014 eclipse of the complex binary EE Cephei

Boyd, David
Abstract: We report photometric and spectroscopic observations of the 2014 eclipse of EE Cep. This proved to be one of the shallower eclipses on record rather than one of the deepest as predicted. The general shape of the eclipse light curve was similar to that of the 2003 eclipse. The spectral type before and after eclipse was consistent with B5III and became slightly later at mid-eclipse. Total flux in the Ha emission line remained relatively constant through the eclipse.
Full text: http://arxiv.org/abs/1412.5127v1

## 2015A&A.submitted - Spectral and spatial imaging of the Be+sdO binary phi Persei

D. Mourard, J. D. Monnier, A. Meilland, D. Gies, F. Millour, M. Benisty, X. Che, E. D. Grundstrom, R. Ligi, G. Schaefer, F. Baron, S. Kraus, M. Zhao, E. Pedretti, P. Berio, J.M. Clausse, N. Nardetto, K. Perraut, A. Spang, P. Stee, I. Tallon-Bosc, H. McAlister, T. ten Brummelaar, S.T. Ridgway, J. Sturmann, L. Sturmann, N. Turner, C. Farrington
Abstract: The rapidly rotating Be star phi Persei was spun up by mass and angular momentum transfer from a now stripped-down, hot subdwarf companion. Here we present the first high angular resolution images of phi Persei made possible by new capabilities in longbaseline interferometry at near-IR and visible wavelengths. We observed phi Persei with the MIRC and VEGA instruments of the CHARA Array. Additional MIRC-only observations were performed to track the orbital motion of the companion, and these were fit together with new and existing radial velocity measurements of both stars to derive the complete orbital elements and distance. The hot subdwarf companion is clearly detected in the near-IR data at each epoch of observation with a flux contribution of 1.5% in the H band, and restricted fits indicate that its flux contribution rises to 3.3% in the visible. A new binary orbital solution is determined by combining the astrometric and radial velocity measurements. The derived stellar masses are 9.6+-0.3Msol and 1.2+-0.2Msol for the Be primary and subdwarf secondary, respectively. The inferred distance (186 +- 3 pc), kinematical properties, and evolutionary state are consistent with membership of phi Persei in the alpha Per cluster. From the cluster age we deduce significant constraints on the initial masses and evolutionary mass transfer processes that transformed the phi Persei binary system. The interferometric data place strong constraints on the Be disk elongation, orientation, and kinematics, and the disk angular momentum vector is coaligned with and has the same sense of rotation as the orbital angular momentum vector. The VEGA visible continuum data indicate an elongated shape for the Be star itself, due to the combined effects of rapid rotation, partial obscuration of the photosphere by the circumstellar disk, and flux from the bright inner disk.
Full text: http://fr.arxiv.org/abs/1503.03423

## 2015A&A...575A..99R - Spectroscopic variability of two Oe stars

Rauw, G.; Morel, T.; Nazé, Y.; Eversberg, T.; Alves, F.; Arnold, W.; Bergmann, T.; Correia Viegas, N. G.; Fahed, R.; Fernando, A.; González-Pérez, J. N.; Gouveia Carreira, L. F.; Hempelmann, A.; Hunger, T.; Knapen, J. H.; Leadbeater, R.; Marques Dias, F.; Mittag, M.; Moffat, A. F. J.; Reinecke, N.; Ribeiro, J.; Romeo, N.; Sánchez Gallego, J.; Dos Santos, E. M.; Schanne, L.; Schmitt, J. H. M. M.; Schröder, K.-P.; Stahl, O.; Stober, Ba.; Stober, Be.; Vollmann, K.
Abstract: Context. The two Oe stars HD 45 314 and HD 60 848 have recently been found to exhibit very different X-ray properties: whilst HD 60 848 has an X-ray spectrum and the emission level typical of most OB stars, HD 45 314 features a much harder and brighter X-ray emission, making it a so-called gamma Cas analogue. Aims: Monitoring the optical spectra could provide hints towards the origin of these very different behaviours. Methods: We analyse a large set of spectroscopic observations of HD 45 314 and HD 60 848, extending over 20 years. We further attempt to fit the Halpha line profiles of both stars with a simple model of emission line formation in a Keplerian disk. Results: Strong variations in the strengths of the Halpha, Hbeta, and He i lambda 5876 emission lines are observed for both stars. In the case of HD 60 848, we find a time lag between the variations in the equivalent widths of these lines, which is currently not understood. The emission lines are double peaked with nearly identical strengths of the violet and red peaks. The Halpha profile of this star can be successfully reproduced by our model of a disk seen under an inclination of 30°. In the case of HD 45 314, the emission lines are highly asymmetric and display strong line profile variations. We find a major change in behaviour between the 2002 outburst and the one observed in 2013. This concerns both the relationship between the equivalent widths of the various lines and their morphologies at maximum strength (double-peaked in 2002 versus single-peaked in 2013). Our simple disk model fails to reproduce the observed Halpha line profiles of HD 45 314. Conclusions: Our results further support the interpretation that Oe stars do have decretion disks similar to those of Be stars. Whilst the emission lines of HD 60 848 are explained well by a disk with a Keplerian velocity field, the disk of HD 45 314 seems to have a significantly more complex velocity field that could be another signature of the phenomenon that produces its peculiar X-ray emission.
Full text: http://arxiv.org/abs/1501.01377

## 2014arxiv1411.6165 - Magnetic fields of Be stars: preliminary results from a hybrid analysis of the MiMeS sample

G.A. Wade, V. Petit, J. Grunhut, C. Neiner
Abstract: In the context of the MiMeS survey of magnetism in massive stars, 85 classical Be stars were observed in circular polarization with the aim of detecting magnetic fields at their surfaces. No direct evidence of such fields is found, in contrast to the significant rate of detection (5-10\%) in non-Be B-type stars. In this paper we describe the sample properties, the methodology and the data quality. We describe a novel method, previously applied to Herbig Ae/Be stars, that allows us to infer upper limits on organized (dipolar) magnetic fields present in the photospheres of our targets. We review the characteristics and robustness of this null result, and discuss its implications.
Full text: http://arxiv.org/abs/1411.6165v1

## 2014MNRAS.submitted - K I 7699 A and related shell lines during the recent eclipse of epsilon Aurigae

C. Muthumariappan, M. Parthasarathy, R. Leadbeater, I.S. Potravnov, M. Appakutty, K. Jayakumar
Abstract: We report high-resolution (R = 30\ 000, 45\ 000 and 75\ 000) echelle and medium-resolution (R = 22\ 000 and 10\ 000) spectroscopic observations of the long-period, eclipsing binary ? Aurigae during the 2009 - 2011 eclipse. Low-excitation shell lines, viz, the K {\sevensize \rm I} line at 7699 \AA\ (with 346 data points), Cr {\sevensize \rm I} lines at 5345.807 \AA\ and 5348.326 \AA\ and Fe {\sevensize \rm I} line at 5110.435 \AA\ which originated from the disk shaped secondary, Ha and the shell components of the Na D1 and D2 lines show significant variation in their shapes and radial velocities during the eclipse. The equivalent width curve shown by the K {\sevensize \rm I} line around the ingress and egress phases indicates that the gas density in the trailing edge is about a factor of two higher than the density in the leading edge. Using a geometrical model, in which a homogeneous, cylindrical Keplarian disk eclipses the F0Ia primary star and the shell absorption lines originate from the gaseous atmosphere around an opaque disk, we fit the equivalent width and the radial velocity curves of the K {\sevensize \rm I} line covering the full eclipse. A reasonably good fit can be achieved by a low-mass binary model where the mass of the central star of the disk is 5.4 M? and the mass of the primary is 2.5 M? and a disk size of 8.9 AU. The low-mass of the primary, with enhanced s-process elements found by Sadakane et al. (2010), supports that it is a post-AGB F supergiant. For the high-mass binary model, the modelled radial velocity curve deviates significantly from the observations.
Full text: http://arxiv.org/abs/1409.5493

## 2014NATURE13834 - The expanding fireball of Nova Delphini 2013

G. H. Schaefer, T. ten Brummelaar, D. R. Gies, C. D. Farrington, B. Kloppenborg, O. Chesneau, J. D. Monnier, S. T. Ridgway, N. Scott, I. Tallon-Bosc, H. A. McAlister, T. Boyajian, V. Maestro, D. Mourard, A. Meilland, N. Nardetto, P. Stee, J. Sturmann, N. Vargas, F. Baron, M. Ireland, E. K. Baines, X. Che, J. Jones, N. D. Richardson, R. M. Roettenbacher, L. Sturmann, N. H. Turner, P. Tuthill, G. van Belle, K. von Braun, R. T. Zavala, D. P. K. Banerjee, N. M. Ashok, V. Joshi, J. Becker & P. S. Muirhead
Abstract: A classical nova occurs when material accreting onto the surface of a white dwarf in a close binary system ignites in a thermonuclear runaway1,2.Complex structures observed in the ejecta at late stages3–5 could resultfrominteractions with thecompanionduring thecommonenvelope phase6,7. Alternatively, the explosion could be intrinsically bipolar, resulting froma localized ignition on the surface of thewhite dwarf8 or as a consequence of rotational distortion9,10. Studying the structure of novae during the earliest phases is challenging because of the high spatial resolution needed to measure their small sizes11. Here we report near-infrared interferometric measurements of the angular size of Nova Delphini 2013, starting one day after the explosion and continuing with extensive time coverage during the first 43 days. Changes in the apparent expansion rate can be explained by an explosion model consisting of an optically thick core surrounded by adiffuse envelope.The opticaldepth of the ejected material changes as it expands. We detect an ellipticity in the light distribution, suggesting a prolate or bipolar structure that develops as early as the second day.Combining the angular expansion rate with radial velocity measurements, we derive a geometric distance to the nova of 4.5460.59 kiloparsecs from the Sun.
Full text: http://www.nature.com/nature/journal/vaop/ncurrent/full/nature13834.html#figures

## 2014MNRAS.441.1435L - Historical vanishing of the Blazhko effect of RR Lyr from the GEOS and Kepler surveys

Le Borgne, J. F.; Poretti, E.; Klotz, A.; Denoux, E.; Smith, H. A.; Kolenberg, K.; Szabó, R.; Bryson, S.; Audejean, M.; Buil, C.; Caron, J.; Conseil, E.; Corp, L.; Drillaud, C.; de France, T.; Graham, K.; Hirosawa, K.; Klotz, A. N.; Kugel, F.; Loughney, D.; Menzies, K.; Rodríguez, M.; Ruscitti, P. M.
Abstract: RR Lyr is one of the most studied variable stars. Its light curve has been regularly monitored since the discovery of its periodic variability in 1899. The analysis of all observed maxima allows us to identify two primary pulsation states, defined as pulsation over a long (P0 longer than 0.56684 d) and a short (P0 shorter than 0.56682 d) primary pulsation period. These states alternate with intervals of 13-16 yr, and are well defined after 1943. The 40.8-d periodical modulations of the amplitude and the period (i.e. the Blazhko effect) were noticed in 1916. We provide homogeneous determinations of the Blazhko period in the different primary pulsation states. The Blazhko period does not follow the variations of P0 and suddenly diminished from 40.8 d to around 39.0 d in 1975. The monitoring of these periodicities deserved, and still deserves, a continuous and intensive observational effort. For this purpose, we have built dedicated, transportable and autonomous small instruments, Very Tiny Telescopes (VTTs), to observe the times of maximum brightness of RR Lyr. As immediate results, the VTTs recorded the last change of the P0 state in mid-2009 and extended the time coverage of the Kepler observations, thus recording a maximum O - C amplitude of the Blazhko effect at the end of 2008, followed by the historically smallest O - C amplitude in late 2013. This decrease is still ongoing and the VTTs are ready to monitor the expected increase in the next few years.
Full text: http://arxiv.org/pdf/1405.3854v1

## 2014MNRAS.440.1674H - Amplitude variability in satellite photometry of the non-radially pulsating O9.5 V star zeta Oph

Howarth, Ian D.; Goss, K. J. F.; Stevens, I. R.; Chaplin, W. J.; Elsworth, Y.
Abstract: We report a time series analysis of satellite photometry of the non-radially pulsating Oe star zeta Oph, principally using data from the Solar Mass Ejection Imager obtained during 2003-2008, but augmented with Microvariability and Oscillations of STars and Wide-field InfraRed Explorer results. Amplitudes of the strongest photometric signals, at 5.18, 2.96 and 2.67 d-1, each vary independently over the 51/2-year monitoring period (from ˜50 to ?2 mmag at 5.18 d-1), on time-scales of hundreds of days. Signals at 7.19 and 5.18 d-1 have persisted (or recurred) for at least two decades. Supplementary spectroscopic observations show an Halpha emission episode in 2006; this coincided with small increases in amplitudes of the three strongest photometric signals.
Full text: http://arxiv.org/pdf/1402.6551v2

## 2014JBAA..124..267B - Spectroscopic observations of the bright RV Tauri variable R Scuti

Boyd, David
Abstract: A series of spectra of the RV Tauri star R Scuti taken as it rose from a deep minimum to a bright maximum during 2013 October and November reveals major changes taking place in the photosphere and outer atmosphere of the star. This may be the first such series of spectra and demonstrates the capability of amateur spectroscopy for studying these complex stars.
Full text: http://arxiv.org/abs/1409.8598v1

## 2014IBVS.6109....1P - Long-term monitoring of Halpha emission strength and photometric V magnitude of gamma Cas

Pollmann, E.; Vollmann, W.; Henry, G. W.

Full text: http://www.konkoly.hu/cgi-bin/IBVSpdf?6109

## 2014IBVS.6103....1P - Periodic Behaviour of the HeI 6678 A Emission Line in gamma Cas

Pollmann, Ernst; Guarro Flo, Joan

Full text: http://www.konkoly.hu/cgi-bin/IBVSpdf?6103

## 2014ATel.6684....1 - Spectroscopic classification of ASASSN-14jv as a cataclysmic variable in outburst

Paolo Berardi
Abstract: We report an optical spectrogram of ASASSN-14jv (ATel #6676, #6680), obtained on November 10.7 UT with a 23 cm Schmidt-Cassegrain telescope and Lhires III spectrograph configured for low-resolution (range 420-710 nm, resolution 1 nm). The strong blue continuum, a weak and narrow emission for H-alpha and other Balmer lines in broadened absorption suggest that the transient is a dwarf nova outburst.

## 2014ATel.6380....1T - The stability of the He II 4686 line emission across periastron passages in eta Carinae

Teodoro, Mairan; Heathcote, Bernard; Richardson, Noel; Prates, Rodrigo; Damineli, Augusto; Hickel, Gabriel; Bohlsen, Terry; Luckas, Paul; Locke, Malcolm; Navarete, Felipe; West, Julian; Andrade, Thiago A.; Coimbra, Adriano M.; Fernandez-Lajus, Eduardo; Gull, Theodore; Jablonski, Francisco; Corcoran, Michael F.; Groh, Jose H.; Hamaguchi, Kenji; Madura, Thomas; St-Jean, Lucas; Weigelt, Gerd
Abstract: Preliminary analysis of data from the international campaign to monitor eta Carinae through the 2014 event shows that, as expected, the equivalent width of the He II 4686 emission line has reached its minimum strength on JD=2456870.8 (August 01 2014).

## 2014ATel.6380....1T - He II 4686 in eta Carinae: no significant changes between 2009.0 and 2014.6

Teodoro, Mairan; Heathcote, Bernard; Richardson, Noel; Prates, Rodrigo; Damineli, Augusto; Hickel, Gabriel; Bohlsen, Terry; Luckas, Paul; Locke, Malcolm; Navarete, Felipe; West, Julian; Andrade, Thiago A.; Coimbra, Adriano M.; Fernandez-Lajus, Eduardo; Gull, Theodore; Jablonski, Francisco; Corcoran, Michael F.; Groh, Jose H.; Hamaguchi, Kenji; Madura, Thomas; St-Jean, Lucas; Weigelt, Gerd
Abstract: In summary, judging from the timing, strength, and overall behavior of the equivalent width of the He II 4686, we can conclude that no significant changes have occurred between the 2009.0 and 2014.6 events, i.e., the two passages produced amazingly similar results.

## 2014ATel.6362....1D - Transition of the H-alpha line from absorption to a double-peaked emission in the Be star HD 224544

Desnoux, V.
Abstract: We report the observation of an emission event in H-alpha for the Be star HD 224544. Spectra were obtained at the Observatoire de Haute Provence, France, with a 0.2m telescope and a Lhires III spectrograph.

## 2014ATel.6355....1C - Observations of rapid line variations of the Halpha line of SS 433 following a large optical flare

Charbonnel, S.; Garde, O.; Edlin, J.
Abstract: Following the announcement of an extreme outburst of SS 433 (#ATel 6347) we observed the source between 3800 - 7500A at a resolution of ~600. All observations reported here were obtained on consecutive nights, 2014 Jul.

## 2014ATel.6258....1B - Spectroscopic classification of ASASSN-14cv as a cataclysmic variable in outburst

Berardi, Paolo; Lester, Tim; Teyssier, Francois
Abstract: We obtained two low-resolution optical spectra of ASASSN-14cv (vsnet-alert 17395, vsnet-alert 17402, vsnet-alert 17404) on June 22.9 UT using a 0.23-m Schmidt-Cassegrain telescope, Lhires III spectrograph configured for low-resolution

## 2014ATel.6235....1T - Spectroscopic classification of ASASN-14cl as a cataclysmic variable in outburst

Teyssier, Francois
Abstract: We report than an optical spectrogram of ASASSN-14cl (ATel #6233) shows that it is a dwarf nova outburst, as suggested by Stanek et al. (2014). The spectrum obtained on June 15.0 UT (range 400-680 nm, resolution 0.6 nm) with a 25 cm SC10" telescope and slit spectrograph LISA (R = 1000, 9 x 300 sec exposures) shows a strong blue continuum, narrow component in a broad absorption for H alpha, other Balmer lines in absorption and He II 4686 in emission.

## 2014ATel.6132....1S - The first detection of the Raman scattered O VI 1032 A line in classical novae - the case of Nova Del 2013 and Nova Cyg 2014

Skopal, A.; Wolf, M.; Slechta, M.; Teyssier, F.; Montier, J.; Lester, T.; Garde, O.; Buil, C.; Lemoult, T.; Charbonnel, S.
Abstract: We report on a transient emergence of the Raman scattered O VI 1032 A line in the spectrum of classical novae V339 Del (Nova Del 2013) and V2659 Cyg (Nova Cyg 2014).

## 2014AJ.Accepted - High-resolution, H band Spectroscopy of Be Stars with SDSS-III/APOGEE: I. New Be Stars, Line Identifications, and Line Profiles

S. Drew Chojnowski, David G. Whelan, John P. Wisniewski, Steven R. Majewski, Matthew Hall, Matthew Shetrone, Rachael Beaton, Adam Burton, Guillermo Damke, Steve Eikenberry, Sten Hasselquist, Jon A. Holtzman, Szabolcs Meszaros, David Nidever, Donald P. Schneider, John Wilson, Gail Zasowski, Dmitry Bizyaev, Howard Brewington, J. Brinkmann, Garrett Ebelke, Peter M. Frinchaboy, Karen Kinemuchi, Elena Malanushenko, Viktor Malanushenko, Moses Marchante, Daniel Oravetz, Kaike Pan, Audrey Simmons
Abstract: APOGEE has amassed the largest ever collection of multi-epoch, high-resolution (R~22,500), H-band spectra for B-type emission line (Be) stars. The 128/238 APOGEE Be stars for which emission had never previously been reported serve to increase the total number of known Be stars by ~6%. We focus on identification of the H-band lines and analysis of the emission peak velocity separations (v_p) and emission peak intensity ratios (V/R) of the usually double-peaked H I and non-hydrogen emission lines. H I Br11 emission is found to preferentially form in the circumstellar disks at an average distance of ~2.2 stellar radii. Increasing v_p toward the weaker Br12--Br20 lines suggests these lines are formed interior to Br11. By contrast, the observed IR Fe II emission lines present evidence of having significantly larger formation radii; distinctive phase lags between IR Fe II and H I Brackett emission lines further supports that these species arise from different radii in Be disks. Several emission lines have been identified for the first time including ~16895, a prominent feature in the spectra for almost a fifth of the sample and, as inferred from relatively large v_p compared to the Br11-Br20, a tracer of the inner regions of Be disks. Unlike the typical metallic lines observed for Be stars in the optical, the H-band metallic lines, such as Fe II 16878, never exhibit any evidence of shell absorption, even when the H I lines are clearly shell-dominated. The first known example of a quasi-triple-peaked Br11 line profile is reported for HD 253659, one of several stars exhibiting intra- and/or extra-species V/R and radial velocity variation within individual spectra. Br11 profiles are presented for all discussed stars, as are full APOGEE spectra for a portion of the sample.
Full text: http://arxiv.org/abs/1409.4668v1

## 2014A&A...567A..57K - HD 161306: a radiatively interacting Be binary?

Koubský, P.; Kotková, L.; Kraus, M.; Yang, S.; Slechta, M.; Harmanec, P.; Wolf, M.; Votruba, V.; Kubát, J.; Kubátová, B.; Niemczura, E.; Skoda, P.
Abstract: The spectrum of the Be star HD 161306 is shown to vary periodically with a period of ~100 days. The radial velocity of the He i 6678 Å emission peak varying in antiphase to the radial velocity of the Halpha emission wings component suggests that the star is a binary similar to phi Per, 59 Cyg, or FY CMa, i.e. a radiatively interacting Be binary - a rare case among Be stars. This type of object is also called a phi Per-type binary or Be + sdO binaries. The range of radial-velocity variations of the strong emission peak in the helium line observed in HD 161306 is about 180 km s-1, similar to what is observed for these systems. We therefore conclude that HD 161306 may represent another case of a Be star with a hot subdwarf companion. Based on observations obtained with the Perek 2-m Telescope at Ondrejov Observatory, Czech Republic, and with the 1.22-m Telescope of the Dominion Astrophysical Observatory, Canada. This work made use of the BeSS database, operated at LESIA, Observatoire de Meudon, France.The spectra taken in Ondrejov (Halpha and helium regions) are only available in electronic form (FITS format) at the CDS via anonymous ftp to http://cdsarc.u-strasbg.fr (ftp://130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/567/A57

## 2013JBAA..123..366P - Spectroscopic observations of the outburst of SS Cygni in September-October 2013

Boyd, David

Full text: http://www.britastro.org/jbaa/pdf_cut/jbaa_3235.pdf

## 2013JBAA..123..302P - Spectroscopic observations of Nova Delphini 2013

Boyd, David

Full text: http://www.britastro.org/jbaa/pdf_cut/jbaa_3200.pdf

## 2013JBAA..123..116P - CCD and spectroscopic observations of Nova Cephei 2013

Boyd, David

Full text: http://www.britastro.org/journal_old/pdf/123-2forum.pdf

## 2013JAVSO..41..182M - Discovery of Pulsating Components in the Southern Eclipsing Binary Systems AW Velorum, HM Puppis, and TT Horologii

Moriarty, D. J. W.; Bohlsen, T.; Heathcote, B.; Richards, T.; Streamer, M.
Abstract: Eclipsing binary stars with pulsating components are especially valuable for studies of stellar evolution. We have discovered that three eclipsing binary stars in the southern sky have a pulsating component with oscillations similar to those of delta Scuti stars. The systems are: AW Velorum, HM Puppis, and TT Horologii. Their spectral types were determined as A7 for AW Vel and HM Pup and F0-F2 for TT Hor. The dominant pulsation frequencies are 15-38 cycles per day with amplitudes of 10-60 millimagnitudes.
Full text: http://www.aavso.org/sites/default/files/jaavso/ej241.pdf

## 2013JAVSO..41...24P - Intermediate Report on January 2013 Campaign: Photometry and Spectroscopy of P Cygni

Pollmann, E., Vollmann, W.
Abstract: In this campaign on the Luminous Blue Variable star P Cygni, we are trying for the first time, by way of contemporaneous measurements of photometric V brightness and HÎ± equivalent width (EW), to realize a long-term monitoring of the intrinsic HÎ± line flux. Photometric and spectroscopic observers started this campaign in November 2008 in order to continue former investigations whose results are based on multi-daily averaging of V and EW. The campaign results enable us to represent the quantitative behavior of the HÎ± line flux for the time span August 2005 to December 2011, which reflects variabilities in mass-loss rate, stellar wind density, and the ionization structure.
Full text: http://www.aavso.org/sites/default/files/jaavso/v41n1/24.pdf

## 2013IBVS.6060....1C - Photometric and spectroscopic variations of the Be star HD 112999

Corti, M. A.; Gamen, R. C.; Aidelman, Y. J.; Ferrero, G. A.; Weidmann, W. A.
Abstract: general Be objects are stars of B spectral type showing lines of the Balmer series in emission. The presence of these lines is attributed to the existence of an extended envelope, disk type, around them. Some stars are observed in both the Be and normal B-type spectroscopic states and they are known as transient Be stars. In this paper we show the analysis carried out on a new possible transient Be star, labelled HD 112999, using spectroscopic optical observations and photometric data.
Full text: http://arxiv.org/pdf/1305.7098v1

## 2013CEAB...37..207N - An Unusual Quadruple System xi Tauri

Nemravová, J. A.; Harmanec, P.; Bencheikh, J.; Bolton, C. T.; Bozicc, H.; Broz, M.; Engle, S.; Grunhut, J.; Guinan, E. F.; Hummel, C. A.; Korcáková, D.; Koubský, P.; Mayer, P.; Mourard, D.; Ribeiro, J.; Slechta, M.; Vokrouhlický, D.; Votruba, V.; Wolf, M.; Zasche, P.; Chara/Vega Team; Npoi Team
Abstract: A preliminary analysis of spectroscopic, photometric and interferometric observations of the triple subsystem of a hierarchical quadruple system xi Tau is presented. The triple system consists of a close eclipsing binary (P^{A} = 7fd146651), revolving around a common centre of gravity with a distant tertiary (P^{B} = 145.17&d). All three stars have comparable brightness. The eclipsing pair consists of two slowly-rotating A stars while the tertiary is a rapidly-rotating B star. The outer orbit is eccentric (e^{B} = 0.237 ± 0.022). Available electronic radial velocities indicate an apsidal advance of the outer orbit with a period P_{APS}^{B} = 224 ± 147 yr.

## 2013CEAB...37...99H - A New Look into the Spectral and Light Variations of epsilon Aur

Harmanec, P.; Bozic, H.; Korcáková, D.;Kotková, L.; Skoda, P.; Slechta, M.; Svanda, M.; Votruba, V.; Wolf, M.; Zasche, P.; Henden, A.; Ribeiro, J.
Abstract: Investigating long series of spectral and photometric observations, we found that the orbital elements of epsilon Aur are subject to much larger uncertainties than usually believed. The Halpha emission is found to move basically with the F primary but its exact location should still be investigated. We also find strong additional absorption and large reddening of the object near the third contact during the eclipse. Episodic atmospheric mass transfer from the F primary towards its companion is tentatively suggested.

## 2013CEAB...37...73R - Recent Observations of zeta Tau

Ruzdjak, D.; Pollmann, E.; Bozic, H.
Abstract: We report a recent decrease of the Halpha emission strength in a bright Be shell star zeta Tau. The decrease of emission is caused presumably by depletion of the material in the circumstellar disc which resulted in disappearance of pronounced long term radial velocity and V/R variations. The period analysis of the equivalent width data gives the period of 132 days for the Halpha equivalent width and about 70 days for the He I 6678 Ar line.

## 2013CEAB...37...67G - Spectroscopy of the Mysterious Be System FF Cam

Garrel, T.; Miroshnichenko, A. S.; Danford, S.; Charbonnel, S.; Houpert, F.; Grankin, K. N.; Kusakin, A. V.
Abstract: FF Cam is a variable star near the North celestial pole with hydrogen lines in emission. Its optical variability of ˜0.3 mag was discovered by HIPPARCOS. The spectral type assigned to the star in SIMBAD is B9, but its position coincides with a ROSAT X--ray source. This suggests the presence of a high-temperature region in the system that could originate at or near a companion object. We undertook a spectroscopic monitoring of FF Cam since the beginning of 2012 and found an extremely variable Halpha line profile as well as periodically variable radial velocities of numerous absorption lines. The main conclusion from our study is that FF Cam is a binary system with an orbital period of 7.785 days, a B--type primary and a K--type secondary component. We discuss the spectral features, their variations, and the nature of FF Cam.

## 2013CBET.3542....1Y - Nova Scorpii 2013 = Psn J17335943-3606216

Yusa, T.; Waagen, E.; Amorim, A.; Buil, C.

Full text: http://www.cbat.eps.harvard.edu/iau/cbet/003500/CBET003542.txt

## 2013BAVSR..62..105R - Neuere Beobachtungen am Be-Doppelstern Zeta Tauri

Ruzdjak, D.; Pollmann, Ernst; Bozic, H.
Abstract: We report about new photometry and spectral analysis of the well observed Be star Zeta Tau. He shows evident variations of brightness, spectra and of his color. Zeta Tau is also a spectroscopic binary with a period of 133 days, his radial velosity indicates longtime variations.
Full text: http://www.bav-astro.de/rb/rb2013-2/105.pdf

## 2013ATel.5546....1S - Continuing spectroscopic observations (3600-8800A) of V339 Del = Nova Del 2013 in the early nebular stage with the Nordic Optical Telescope, Ondrejov Observatory and the ARAS group

Shore, S. N.; Cechura, J.; Korcakova, D.; Kubat, J.; Skoda, P.; Slechta, M.; Votruba, V.; Alton, K.; Antao, D.; Barbotin, E.; Berardi, P.; Blank, T.; Bohlsen, P.; Boubault, F.; Boyd, D.; Briol, J.; Buchet, Y.; Buil, C.; Charbonnel, S.; Dubreuil, P.; Dubs, M.; Edlin, J.; France, T. de; Favaro, A.; Gerlach, P.; Garde, O.; Graham, K.; Greenan, D.; Guarro, J.; Hansen, T.; Hyde, D.; Lemoult, T.; Leadbeater, R.; Martineau, G.; Masviel, J. P.; Mauclaire, B.; Montier, J.; Pollmann, E.; Potter, M.; Ribeiro, J.; Schramm, B.; Thizy, O.; Terry, J.-N.; Teyssier, F.
Abstract: We have been continuing almost nightly spectroscopic observations of V339 Del (see ATel#5378) with the 2.6 m Nordic Optical Telecope (NOT) FIbre-fed Echelle Spectrograph (FIES) (R ~ 67000), the Ondrejov Observatory 2m Zeiss coude spectrograph (R = 18000), and a variety of grating and echelle spectrographs of the ARAS group in the wavelength range 3684 - 7431A with resolutions ranging from 580 - 12000.

## 2013ATel.5409....1S - First high resolution ultraviolet (HST/STIS) and supporting optical spectroscopy of V339 Del = Nova Del 2013

Shore, S. N.; Schwarz, G. J.; Alton, K.; Antao, D.; Barbotin, E.; Berardi, P.; Blank, T.; Bohlsen, T.; Boubault, F.; Boyd, D.; Briol, J.; Buil, C.; Charbonnel, S.; Dubreuil, P.; Dubs, M.; Edlin, J.; de France, T.; Favaro, A.; Garde, O.; Graham, K.; Greenan, D.; Guarro, J.; Hansen, T.; Hyde, D.; Lemoult, T.; Leadbeater, R.; Martineau, G.; Buchet, Y.; Masviel, J. P.; Montier, J.; Mauclaire, B.; Pollmann, E.; Ribeiro, J.; Schram, B.; Thizy, O.; Terry, J.-N.; Teyssier, F.; Page, K. L.; Osborne, J. P.; Ness, J.-U.; Starrfield, S.; Walter, F. M.; Woodward, C. E.; Bode, M. F.
Abstract: V339 Del = Nova Del 2013 was observed with the Space Telescope Imagine Spectrograph (STIS) aboard the Hubble Space Telescope (HST) on 2013 Sept. 18.2 UT from 1140-2888 A using the E140M and G230H gratings at a resolution of ~ 100000. At the time, V ~ 8, shortly after t_3. Continuing spectroscopy was provided by the Astronomical Ring for Access to Spectroscopy (ARAS) at resolutions ranging from 3684 - 7431 A with resolutions ranging from 580 - 11000 with time sequences as short as 10 minutes at resolutions up to 12000.

## 2013ATel.5378....1S - Continuing optical spectroscopy of V339 Del = Nova Del 2013 with the Nordic Optical Telescope and the ARAS Group

Shore, S. N.; Alton, K.; Antao, D.; Barbotin, E.; Berardi, P.; Bohlsen, P.; Boubault, F.; Boyd, D.; Briol, J.; Buil, C.; Charbonnel, S.; Dubreuil, P.; Dubs, M.; Edlin, J.; de France, T.; Favaro, A.; Garde, O.; Graham, K.; Greenan, D.; Guarro, J.; Hansen, T.; Hyde, D.; Lemoult, T.; Leadbeater, R.; Martineau, G.; Buchet, Y.; Masviel, J. P.; Montier, J.; Pollmann, E.; Ribeiro, J.; Thizy, O.; Terry, J.-N.; Teyssier, F.
Abstract: Since our first report (ATel#5312) we have been continuing nightly, almost hourly spectroscopic observations of V339 Del = Nova Del 2013 = PNV J20233073+2046041). Here we report the state at approximately the t_3 point in the photometric decline (see also ATel#5370). Spectra have been obtained with the 2.6 m Nordic Optical Telecope FIbre-fed Echelle Spectrograph (FIES) (R ~ 67000), the Ondrejov Observatory 2m Zeiss coude spectrograph (R = 18000), and a variety of grating and echelle spectrographs of the ARAS group with resolutions ranging from 580 - 11000.

## 2013ATel.5312....1S - Continuing spectroscopic observations (3500-8800A) of Nova Del 2013 with the Ondrejov Observatory and the ARAS group

Shore, S. N.; Skoda, P.; Korcakova, D.; Kíek, P. Koubsky R.; Rutsch, P.; Slechta, M.; Garde, O.; Thizy, O.; de France, T.; Antao, D.; Edlin, J.; Graham, K.; Guarro, J.; Teyssier, F.; Berard, P.; Bohlsen, i. T.; Pollmann, E.; Lemoult, T.; Favaro, A.; Terry, J.-N.; Barbotin, E.; Boubault, F.; Masviel, J. P.; Leadbeater, R.; Buil, C.; Mauclaire, B.
Abstract: Observations with the Ondrejov Observatory 2m Zeiss coude spectrograph (R = 18000) are continuing covering the range 3550 - 8870 A (see ATel #5282). High cadence spectroscopic monitoring by the Astronomical Ring for Access to Spectroscopy (ARAS) began on 2013 Apr. 14.8 and has continued uninterrupted covering the wavelength interval at resolutions ranging from 3684 - 7431 A with resolutions ranging from 580 - 11000 with time sequences as short as 10 minutes at resolutions up to 12000.

## 2013ASPC..479..319N - Be Star Outbursts: Transport of Angular Momentum by Waves

Neiner, C.; Mathis, S.; Saio, H.; Lee, U.
Abstract: The Be phenomenon, that is the ejection of matter from Be stars into a circumstellar disk, has been a long lasting mystery. In the last few years, the CoRoT (Convection Rotation and planetary Transits) satellite brought clear evidence that Be outbursts are directly correlated with pulsations. We found that it may be the transport of angular momentum by waves or pulsation modes that brings the already rapid stellar rotation to its critical value at the surface, and allows the star to eject material. The recent discovery of stochastically excited gravito-inertial modes by CoRoT in a hot Be star strengthens this scenario. We present the CoRoT observations and modeling of several Be stars and describe the new picture of the Be phenomenon which arose from these results.
Full text: http://arxiv.org/pdf/1311.2411v1

## 2013ApJ...766..119M - The 2011 Periastron Passage of the Be Binary delta Scorpii

Miroshnichenko, A. S.; Pasechnik, A. V.; Manset, N.; Carciofi, A. C.; Rivinius, Th.; Stefl, S.; Gvaramadze, V. V.; Ribeiro, J.; Fernando, A.; Garrel, T.; Knapen, J. H.; Buil, C.; Heathcote, B.; Pollmann, E.; Mauclaire, B.; Thizy, O.; Martin, J.; Zharikov, S. V.; Okazaki, A. T.; Gandet, T. L.; Eversberg, T.; Reinecke, N.
Abstract: We describe the results of the world-wide observing campaign of the highly eccentric Be binary system delta Scorpii 2011 periastron passage which involved professional and amateur astronomers. Our spectroscopic observations provided a precise measurement of the system orbital period at 10.8092 ± 0.0005 yr. Fitting of the He II 4686 Å line radial velocity curve determined the periastron passage time on 2011 July 3, UT 9:20 with a 0.9-day uncertainty. Both these results are in a very good agreement with recent findings from interferometry. We also derived new evolutionary masses of the binary components (13 and 8.2 M &sun;) and a new distance of 136 pc from the Sun, consistent with the HIPPARCOS parallax. The radial velocity and profile variations observed in the Halpha line near the 2011 periastron reflected the interaction of the secondary component and the circumstellar disk around the primary component. Using these data, we estimated a disk radius of 150 R &sun;. Our analysis of the radial velocity variations measured during the periastron passage time in 2000 and 2011 along with those measured during the 20th century, the high eccentricity of the system, and the presence of a bow shock-like structure around it suggest that delta Sco might be a runaway triple system. The third component should be external to the known binary and move on an elliptical orbit that is tilted by at least 40° with respect to the binary orbital plane for such a system to be stable and responsible for the observed long-term radial velocity variations. This paper is partially based on observations obtained at the Canada-France-Hawaii Telescope (CFHT) which is operated by the National Research Council of Canada, the Institut National des Sciences de l'Univers of the Centre National de la Recherche Scientifique de France, and the University of Hawaii, the 2.2 m MPG telescope operated at ESO/La Silla under program IDs 086.A-9019 and 087.A-9005, the IAC80 telescope in the Spanish Observatorio del Teide of the Instituto de Astrofiísica de Canarias, and data from the ELODIE archive at the Observatoire de Haute-Provence.
Full text: http://iopscience.iop.org/0004-637X/766/2/119/pdf/apj_766_2_119.pdf

## 2013ApJ...765....2P - Far-ultraviolet Detection of the Suspected Subdwarf Companion to the Be Star 59 Cygni

Peters, Geraldine J.; Pewett, Tiffany D.; Gies, Douglas R.; Touhami, Yamina N.; Grundstrom, Erika D.
Abstract: We report on the detection of a hot subdwarf component in the Be binary system, 59 Cygni. The spectral signature is found in cross-correlation functions of photospheric model spectra with far-ultraviolet spectra obtained by the International Ultraviolet Explorer Satellite, and we used radial velocities from the cross-correlation functions to determine a double-lined spectroscopic orbit. The individual spectra of the binary components were extracted using a Doppler tomography algorithm. The flux of the system is dominated by the rapidly rotating Be star. However, the subdwarf contributes approximately 4% of the UV flux, and its spectrum bears a strong resemblance to that of the hot sdO star BD +75°325. Based on the appearance of the UV spectrum and the orbital elements, we present estimates for the stellar masses, radii, and temperatures. The presence of the hot companion causes excess emission from the outer part of the Be disk facing the companion. We present a set of red spectra that show the orbital phase variations of the He I lambda6678 emission formed in the heated region of the disk, which probably occurs near the disk outer boundary. 59 Cygni, FY Canis Majoris, and phi Persei comprise the known set of Be binaries with detected hot evolved companions, which are the stripped down remains of mass transfer. Their properties demonstrate that some fraction of Be stars were spun up through angular momentum transfer by Roche lobe overflow.
Full text: http://arxiv.org/pdf/1301.0257v1

## 2013AEC...2942 - NOVA DELPHINI 2013

Garde, Olivier
Abstract: Strong H-alpha emission has been noted by Masi et al. (low-resolution spectra taken with a 36-cm robotic telescope at Ceccano; scale about 3.4nm/pixel; Aug. 14.92 UT) and by Olivier Garde (Observatoire de la Tourbiere, France; C14 telescope; resolution 10000; echelle spectrograph).
Full text: http://www.theastronomer.org/tacirc/2013/e2942.txt

## 2013AASP....3...75D - V407 Cyg and RS Oph - comparison of two exotic variables

Drozd, K.; Swierczynski, E.; Ragan, E.; Buil, C.
Abstract: V407 Cygni and RS Ophiuchi are two similar but unique objects. It can be said that they each belong to an individual type of stars. During their quiet state they seem to be symbiotic stars. However, both stars have previously displayed nova-like outbursts. We would like to take a closer look at these two unique objects, and to compare them. We presented spectroscopic and photometric observations of V407 Cyg and RS Oph obtained throughout the period from 2006 until 2013. Our data show the different activity stages connected with the two components of these binary systems. Multicolour photometry and spectra obtained in a wide frequency range are utilized to understand the behaviour of such extremely binaries.
Full text: http://aasp.kiev.ua/volume3/075-078-Drozd.pdf

## 2013A&ARv..21...69R - Classical Be stars. Rapidly rotating B stars with viscous Keplerian decretion disks

Rivinius, Thomas; Carciofi, Alex C.; Martayan, Christophe
Abstract: In the past decade, a consensus has emerged regarding the nature of classical Be stars: They are very rapidly rotating main sequence B stars, which, through a still unknown, but increasingly constrained process, form an outwardly diffusing gaseous, dust-free Keplerian disk. In this work, first the definition of Be stars is contrasted to similar classes, and common observables obtained for Be stars are introduced and the respective formation mechanisms explained. We then review the current state of knowledge concerning the central stars as non-radially pulsating objects and non-magnetic stars, as far as it concerns large-scale, i.e., mostly dipolar, global fields. Localized, weak magnetic fields remain possible, but are as of yet unproven. The Be-phenomenon, linked with one or more mass-ejection processes, acts on top of a rotation rate of about 75 % of critical or above. The properties of the process can be well constrained, leaving only few options, most importantly, but not exclusively, non-radial pulsation and small-scale magnetic fields. Of these, it is well possible that all are realized: In different stars, different processes may be acting. Once the material has been lifted into Keplerian orbit, memory of the details of the ejection process is lost, and the material is governed by viscosity. The disks are fairly well understood in the theoretical framework of the viscous decretion disk model. This is not only true for the disk structure, but as well for its variability, both cyclic and secular. Be binaries are reviewed under the aspect of the various types of interactions a companion can have with the circumstellar disk. Finally, extragalactic Be stars, at lower metallicities, seem more common and more rapidly rotating.
Full text: http://arxiv.org/pdf/1310.3962v1

## 2013A&A...560A..30Z - Doppler tomography of the circumstellar disk of pi Aquarii

Zharikov, S. V.; Miroshnichenko, A. S.; Pollmann, E.; Danford, S.; Bjorkman, K. S.; Morrison, N. D.; Favaro, A.; Guarro Fló, J.; Terry, J. N.; Desnoux, V.; Garrel, T.; Martineau, G.; Buchet, Y.; Ubaud, S.; Mauclaire, B.; Kalbermatten, H.; Buil, C.; Sawicki, C. J.; Blank, T.; Garde, O.
Abstract: Aims: The work is aimed at studying the circumstellar disk of the bright classical binary Be star pi Aqr. Methods: We analysed variations of a double-peaked profile of the Halpha emission line in the spectrum of pi Aqr that was observed in many phases during ~40 orbital cycles in 2004-2013. We applied the discrete Fourier transform (DFT) method to search for periodicity in the peak intensity ratio (V/R). Doppler tomography was used to study the structure of the disk around the primary. Results: The dominant frequency in the power spectrum of the Halpha V/R ratio is 0.011873 day-1, which corresponds to a period of 84.2(2) days and agrees with the earlier determined orbital period of the system, Porb = 84.1 days. The V/R shows a sinusoidal variation that is phase-locked with the orbital period. Doppler maps of all our spectra show a non-uniform structure of the disk around the primary: a ring with the inner and outer radii at Vin ˜ 450 km s-1 and Vout ˜ 200 km s-1, respectively, along with an extended stable region (spot) at Vx ˜ 225 km s-1 and Vy ˜ 100 km s-1. The disk radius of ˜65 R&sun; = 0.33 AU was estimated by assuming Keplerian motion of a particle on a circular orbit at the disk's outer edge. Table 1 and pi Aquarii spectra in FITS format are only available at the CDS via anonymous ftp to http://cdsarc.u-strasbg.fr (ftp://130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/560/A30 http://www.astrosurf.com/aras/
Full text: http://arxiv.org/pdf/1310.6499v2

## 2013A&A...555A.100D - Spectrally resolved interferometric observations of alpha Cephei and physical modeling of fast rotating stars

Delaa, O.; Zorec, J.; Domiciano de Souza, A.; Mourard, D.; Perraut, K.; Stee, Ph.; Frémat, Y.; Monnier, J.; Kraus, S.; Che, X.; Bério, Ph.; Bonneau, D.; Clausse, J. M.; Challouf, M.; Ligi, R.; Meilland, A.; Nardetto, N.; Spang, A.; McAlister, H.; ten Brummelaar, T.; Sturmann, J.; Sturmann, L.; Turner, N.; Farrington, C.; Goldfinger, P. J.
Abstract: Context. When a given observational quantity depends on several stellar physical parameters, it is generally very difficult to obtain observational constraints for each of them individually. Therefore, we studied under which conditions constraints for some individual parameters can be achieved for fast rotators, knowing that their geometry is modified by the rapid rotation which causes a non-uniform surface brightness distribution. Aims: We aim to study the sensitivity of interferometric observables on the position angle of the rotation axis (PA) of a rapidly rotating star, and whether other physical parameters can influence the determination of PA, and also the influence of the surface differential rotation on the determination of the beta exponent in the gravity darkening law that enters the interpretation of interferometric observations, using alpha Cep as a test star. Methods: We used differential phases obtained from observations carried out in the Halpha absorption line of alpha Cep with the VEGA/CHARA interferometer at high spectral resolution, R = 30 000 to study the kinematics in the atmosphere of the star. Results: We studied the influence of the gravity darkening effect (GDE) on the determination of the PA of the rotation axis of alpha Cep and determined its value, PA = -157-10°+17°. We conclude that the GDE has a weak influence on the dispersed phases. We showed that the surface differential rotation can have a rather strong influence on the determination of the gravity darkening exponent. A new method of determining the inclination angle of the stellar rotational axis is suggested. We conclude that differential phases obtained with spectro-interferometry carried out on the Halpha line can in principle lead to an estimate of the stellar inclination angle i. However, to determine both i and the differential rotation parameter alpha, lines free from the Stark effect and that have collision-dominated source functions are to be preferred.

## 2012SASS...31..105G - High Resolution Spectroscopy for the Amateur: Experiences with the LHIRES III Spectrograph

Gorodenski, Stanley A.
Abstract: This paper describes the author's experience with the high resolution LHIRES III spectrograph and other equipment used. It discusses mechanical improvements made that may have increased the calibration accuracy of the spectrograph, problems with guiding, and the need to take flat fields. It also briefly mentions the freeware software used and the types of computer programs written by the author to aid in the reduction and analysis of the spectra. An assessment is made of the method for determining equivalent width the author described in the 2011 issue of the SAS News. It finishes by illustrating the ability to study binary stars, such as V1143 Cyg, with the LHIRES III, and discusses some interesting results that were obtained on Epsilon Aurigae. The evolution of a split line centered at around 5853 Angstroms is mentioned, as well as other aspects of the Sodium D Lines region, such as the constancy of separation between the two lines.

## 2012MNRAS.427..483B - Multisite spectroscopic seismic study of the beta Cep star V2052 Ophiuchi: inhibition of mixing by its magnetic field

Briquet, M.; Neiner, C.; Aerts, C.; Morel, T.; Mathis, S.; Reese, D. R.; Lehmann, H.; Costero, R.; Echevarria, J.; Handler, G.; Kambe, E.; Hirata, R.; Masuda, S.; Wright, D.; Yang, S.; Pintado, O.; Mkrtichian, D.; Lee, B. C.; Han, I.; Bruch, A.; De Cat, P.; Uytterhoeven, K.; Lefever, K.; Vanautgaerden, J.; de Batz, B.; Frémat, Y.; Henrichs, H.; Geers, V. C.; Martayan, C.; Hubert, A. M.; Thizy, O.; Tijani, A.

Full text: http://arxiv.org/pdf/1208.4250v1.pdf

## 2012MNRAS.426.2738N - An investigation of the magnetic properties of the classical Be star omega Ori by the MiMeS Collaboration

Neiner, C.; Grunhut, J. H.; Petit, V.; ud-Doula, A.; Wade, G. A.; Landstreet, J.; de Batz, B.; Cochard, F.; Gutiérrez-Soto, J.; Huat, A.-L.
Abstract: One hundred and twenty-five new high-precision spectropolarimetric observations have been obtained with ESPaDOnS (Eschelle Spectro-Polarimetric Device for the Observation of Stars) at the Canada-France-Hawaii Telescope and Narval at Télescope Bernard Lyot to investigate the magnetic properties of the classical Be star omega Ori. No Stokes V signatures are detected in our polarimetric data. Measurements of the longitudinal magnetic field, with a median error bar of 30 G, and direct modelling of the mean least-squares deconvolved Stokes V profiles yield no evidence for a dipole magnetic field with polar surface strength greater than ˜80 G. We are therefore unable to confirm the presence of the magnetic field previously reported by Neiner et al. However, our spectroscopic data reveal the presence of periodic emission variability in H and He lines analogous to that reported by Neiner et al., considered as evidence of magnetically confined circumstellar plasma clouds. We revisit this hypothesis in light of the new magnetic analysis. Calculation of the magnetospheric Kepler radius RK and confinement parameter eta* indicates that a surface dipole magnetic field with a polar strength larger than 63 G is sufficient to form of a centrifugally supported magnetosphere around omega Ori. Our data are not sufficiently sensitive to detect fields of this magnitude; we are therefore unable to confirm or falsify the magnetic cloud hypothesis. Based on our results, we examine three possible scenarios that could potentially explain the behaviour of omega Ori: (1) that no significant magnetic field is (or was) present in omega Ori, and that the observed phenomena have their origin in another mechanism or mechanisms than corotating clouds. We are, however, unable to identify one; (2) that omega Ori hosts an intermittent magnetic field produced by dynamo processes; however, no such process has been found so far to work in massive stars and especially to produce a dipolar field; and (3) that omega Ori hosts a stable, organized (fossil) magnetic field that is responsible for the observed phenomena, but with a strength that is below our current detection threshold. Of these three scenarios, we consider the second one (dynamo process) as highly unlikely, whereas the other two should be falsifiable with intense monitoring. Based on observations obtained at the Canada-France-Hawaii Telescope (CFHT) which is operated by the National Research Council of Canada, the Institut National des Sciences de l'Univers of the Centre National de la Recherche Scientifique of France and the University of Hawaii and observations obtained with the Narval spectropolarimeter at the Télescope Bernard Lyot (TBL), Observatoire du Pic du Midi, France.
Full text: http://mnras.oxfordjournals.org/content/426/4/2738.full.pdf+html

## 2012MNRAS.426.2208G - Investigating the spectroscopic, magnetic and circumstellar variability of the O9 subgiant star HD 57682

Grunhut, J. H.; Wade, G. A.; Sundqvist, J. O.; ud-Doula, A.; Neiner, C.; Ignace, R.; Marcolino, W. L. F.; Rivinius, Th.; Fullerton, A.; Kaper, L.; Mauclaire, B.; Buil, C.; Garrel, T.; Ribeiro, J.; Ubaud, S.
Abstract: The O9IV star HD 57682, discovered to be magnetic within the context of the Magnetism in Massive Stars (MiMeS) survey in 2009, is one of only eight convincingly detected magnetic O-type stars. Among this select group, it stands out due to its sharp-lined photospheric spectrum. Since its discovery, the MiMeS Collaboration has continued to obtain spectroscopic and magnetic observations in order to refine our knowledge of its magnetic field strength and geometry, rotational period and spectral properties and variability. In this paper we report new Echelle SpectroPolarimetric Device for the Observation of Stars (ESPaDOnS) spectropolarimetric observations of HD 57682, which are combined with previously published ESPaDOnS data and archival Halpha spectroscopy. This data set is used to determine the rotational period (63.5708 ± 0.0057 d), refine the longitudinal magnetic field variation and magnetic geometry (dipole surface field strength of 880 ± 50 G and magnetic obliquity of 79° ± 4° as measured from the magnetic longitudinal field variations, assuming an inclination of 60°) and examine the phase variation of various lines. In particular, we demonstrate that the Halpha equivalent width undergoes a double-wave variation during a single rotation of the star, consistent with the derived magnetic geometry. We group the variable lines into two classes: those that, like Halpha, exhibit non-sinusoidal variability, often with multiple maxima during the rotation cycle, and those that vary essentially sinusoidally. Based on our modelling of the Halpha emission, we show that the variability is consistent with emission being generated from an optically thick, flattened distribution of magnetically confined plasma that is roughly distributed about the magnetic equator. Finally, we discuss our findings in the magnetospheric framework proposed in our earlier study. Based on observations obtained at the Canada-France-Hawaii Telescope (CFHT) which is operated by the National Research Council of Canada, the Institut National des Sciences de l'Univers of the Centre National de la Recherche Scientifique of France and the University of Hawaii.
Full text: http://arxiv.org/pdf/1207.6988v1

## 2012JAVSO..40..894P - International Observing Campaign: Photometry and Spectroscopy of P Cygni

Pollmann, E.; Bauer, T.
Abstract: In this combined campaign on the Luminous Blue Variable star P Cygni we are trying for the first time by way of contemporaneous measurements of photometric V brightness and Ha equivalent width (EW) to realize a longterm monitoring of the intrinsic Ha-line flux. The photometric observers of AAVSO and BAV (Germany) and a spectroscopic observer group (Japan, France, Spain, Germany) started observing for this campaign in November 2008 at the request of Bernd Hanisch and one of us (EP) in order to continue former investigations whose results were based on multi-daily averaging of V and EW. Additional data from literature enable us to represent the quantitative behavior of the Ha-line flux for the timespan August 2005 to December 2011, which behavior reflects variabilities in mass-loss rate, stellar wind density, and ionization structure.
Full text: http://www.aavso.org/sites/default/files/jaavso/v40n2/894.pdf

## 2012JAVSO..40..743G - Spectroscopic Results From Blue Hills Observatory of the 2009-2011 Eclipse of epsilon Aurigae

Gorodenski, S. A.
Abstract: The purpose of this paper is to report spectroscopic results of epsilon Aurigae during the 2009-2011 eclipse. Spectra of the sodium D lines and an absorption line occurring at approximately 5853Å were taken from February 13, 2010, to October 10, 2011, with an LHIRES III spectrograph and a 16-inch Meade telescope at Blue Hills Observatory in Dewey, Arizona. Equivalent width and radial velocity data support the presence of a void or ring structure within the eclipsing disk, and they support a central disk clearing around an unseen primary central object. The results also indicate the disk does not end at fourth contact but continues for a significant distance. Analysis of radial velocities demonstrated the profile of the 5853Å line has a disk component in addition to the primary F0 star component. A split line at this location was observed. From the equivalent width profile of the 5853Å line the duration of the split line event was estimated to be 101 days. Other lesser results are presented and discussed.
Full text: http://www.aavso.org/sites/default/files/jaavso/v40n2/743.pdf

## 2012JAVSO..40..729L - High Cadence Measurement of Neutral Sodium and Potassium Absorption During the 2009-2011 Eclipse of epsilon Aurigae

Leadbeater, R.; Buil, C.; Garrel, T.; Gorodenski, S. A.; Hansen, T.; Schanne, L.; Stencel, R. E.; Stober, B.
Abstract: The results of a spectroscopic survey of epsilon Aurigae during eclipse using a network of small telescopes are presented. The spectra have a resolution of 0.35 to 0.65Å and cover the period 2008 to 2012 with a typical interval of four days during eclipse. This paper specifically covers variations in the KI 7699Å, Na D, and Mg II 4481Å lines. Absorption started increasing in the KI 7699Å line three months before the eclipse began in optical photometry and had not returned to pre-eclipse levels by the end of the survey in March 2012, seven months after the broadband brightness had returned to normal outside eclipse levels. The contribution of the eclipsing object to the KI 7699Å line has been isolated and shows the excess absorption increasing and decreasing in a series of steps during eclipse ingress and egress. This is interpreted as an indication of structure within the eclipsing object. The F star is totally obscured by the eclipsing object at the Na D wavelength during eclipse. The radial velocity of the F star and the mean and maximum radial velocity of the eclipsing material in front of the F star at any given time have been isolated and tracked throughout the eclipse. The quasi-periodic variations seen in the F star radial velocity (RV) outside eclipse continued during the eclipse. It is hoped that these results can be used to constrain proposed models of the system and its components.
Full text: http://arxiv.org/pdf/1206.6754v1

## 2012JAVSO..40..718M - H-alpha Spectral Monitoring of epsilon Aurigae 2009-2011 Eclipse

Mauclaire, B.; Buil, C.; Garrel, T.; Leadbeater, R.; Lopez, A.
Abstract: We present and analyze epsilon Aurigae data concerning the evolution of the Halpha line on the occasion of the 2009 International observation campaign launched to cover the eclipse of this object. We visually inspect the dynamical spectrum constructed from the data and analyze the evolution with time of the EW (Equivalent Width) and of the radial velocity. The spectroscopic data reveal many details which confirm the complexity of the epsilon Aur system. The object is far from being understood. In particular, according to our measurements, the eclipse duration has been underestimated. A complete analysis of details revealed by our data would require much time and effort. Observers are encouraged to continue monitoring the Ha line out of eclipse in the hope that it will provide further important information
Full text: http://arxiv.org/pdf/1207.0795v2.pdf

## 2012IBVS.6099....5P - Observations of variables

Pollmann, E.; Mauclaire, B.; Bucke, R.

Full text: http://www.konkoly.hu/cgi-bin/IBVSpdf?6099

## 2012IBVS.6034....1P - Non-radial Pulsations of zeta Oph

Pollmann, E.

Full text: http://www.konkoly.hu/cgi-bin/IBVSpdf?6034

## 2012IBVS.6023....1P - Period analysis of the Halpha line profile variation of the Be binary star pi Aqr

Pollmann, Ernst

Full text: http://www.konkoly.hu/cgi-bin/IBVSpdf?6023

Eversberg, T.

## 2012CBET.3282....1K - Supernova 2012fw in ESO 235-G37 = Psn J21015899-4816259

Klotz, A.; Colas, F.; Peyrot, A.; Teng, J. P.; Buil, C.; Chomiuk, L.; Strader, J.; Inserra, C.; Smartt, S. J.; Fraser, M.; Young, D.; Smith, K.; Cellier-Holzem, F.; El-Hage, P.; Pan, Y.-C.; Sullivan, M.; Arcavi, I.; Gal-Yam, A.; Yaron, O.; Benetti, S.; Pastorello, A.; Valenti, S.; Taubenberger, S.; Sternberg, A.; Benitez-Herrera, S.

Full text: http://www.cbat.eps.harvard.edu/iau/cbet/003200/CBET003282.txt

## 2012CBET.3277....3B - Supernova 2012fr in NGC 1365 = Psn J03333599-3607377

Buil, C.

Full text: http://www.cbat.eps.harvard.edu/iau/cbet/003200/CBET003277.txt

## 2012CBET.3277....2K - Supernova 2012fr in NGC 1365 = Psn J03333599-3607377

Klotz, A.; Maury, A.; Childress, M.; Zhou, G.; Tucker, B.; Bayliss, D.; Scalzo, R.; Yuan, F.; Schmidt, B.; Buil, C.

Full text: http://www.cbat.eps.harvard.edu/iau/cbet/003200/CBET003277.txt

## 2012CBET.3276....2K - Supernova 2012fr in NGC 1365 = Psn J03333599-3607377

Klotz, A.; Maury, A.; Childress, M.; Zhou, G.; Tucker, B.; Bayliss, D.; Scalzo, R.; Yuan, F.; Schmidt, B.; Buil, C.

Full text: http://www.cbat.eps.harvard.edu/iau/cbet/003200/CBET003276.txt

## 2012CBET.3275....1K - Supernova 2012fr in NGC 1365 = Psn J03333599-3607377

Klotz, A.; Maury, A.; Childress, M.; Zhou, G.; Tucker, B.; Bayliss, D.; Scalzo, R.; Yuan, F.; Schmidt, B.; Buil, C.

Full text: http://www.cbat.eps.harvard.edu/iau/cbet/003200/CBET003275.txt

## 2012CBET.3202....2W - Nova Monocerotis 2012 = Pnv J06393874+0553520

Waagen, E.; Hambsch, J.; Buil, C.

Full text: http://www.cbat.eps.harvard.edu/iau/cbet/003200/CBET003202.txt

## 2012CBET.3177....4B - Nova Sagittarii 2012 No. 4 = Pnv J18202726-2744263

Buil, C.

Full text: http://www.cbat.eps.harvard.edu/iau/cbet/003100/CBET003177.txt

## 2012CBET.3156....6B - Nova Sagittarii 2012 no. 3 = PNV J17522579-2126215

Buil, C.

Full text: http://www.cbat.eps.harvard.edu/iau/cbet/003100/CBET003156.txt

## 2012CBET.3156....2S - Nova Sagittarii 2012 No. 3 = Pnv J17522579-2126215

Sakurai, Y.; Nakano, S.; Jacques, C.; Pimentel, E.; Yusa, T.; Kiss, L.; Sarneczky, K.; Kovacs, J.; Borkovits, T.; Buil, C.; Itagaki, K.

Full text: http://www.cbat.eps.harvard.edu/iau/cbet/003100/CBET003156.txt

## 2012CBET.3124....1W - Nova Ophiuchi 2012 No. 2 = Pnv J17395600-2447420

Walter, F. M.; Buil, C.

Full text: http://www.cbat.eps.harvard.edu/iau/cbet/003100/CBET003124.txt

## 2012CBET.3089....3B - Nova Sagittarii 2012 = Pnv J17452791-2305213

Buil, C.

Full text: http://www.cbat.eps.harvard.edu/iau/cbet/003000/CBET003089.txt

## 2012BAVSR..61...20P - H-alpha-Emission und v-korrelationen als sonden von be-sternscheiben.

Pollmann, E.; Vollmann, W.; Pusk, S. F.

## 2012BaltA..21..219K - High-Resolution Spectroscopy of the Hydrogen-Deficient Binary Upsilon Sgr

Kipper, Tõnu; Klochkova, Valentina G.
Abstract: The high resolution spectra of hydrogen-deficient binary Upsilon Sgr are analyzed. The atmospheric parameters are T eff=12300± 200 K, log g=2.5±0.5 and xi t=5-15 km s-1 depending on the element. For Fe II xi t=9.3±0.3 km s-1. Iron is slightly underabundant (--0.2 dex). Nitrogen is overabundant with [N/Fe] ˜ 1.0, carbon and oxygen are underabundant with [C/Fe] ˜ --1.6 and [O/Fe] ˜ --1.1. The s-process elements Y, Zr and Ba are overabundant about 0.5 dex. Quite large number of emission lines, both permitted and forbidden, originating from low excitation levels of neutral and ionized metals, are identified. Radial velocities of these emission lines indicate that an accretion disk in the system is present.

## 2012ATel.4310....1C - Possible Association of the Gamma-ray Transient Fermi J0639+0548 with Nova Mon 2012

Cheung, C. C.; Shore, S. N.; De Gennaro Aquino, I.; Charbonnel, S.; Edlin, J.; Hays, E.; Corbet, R. H. D.; Wood, D. L.
Abstract: In ATEL #4224, we reported the detection by the Fermi Large Area Telescope of Fermi J0639+0548, a new gamma-ray transient in the Galactic plane, beginning on 2012 June 22. The transient was seen through the Monoceros region of our Galaxy with Galactic coordinates, (l, b) = (206.42 deg, 0.03 deg). We noted the gamma-ray source was close to the Sun at the time of detection, thus precluding prompt follow-up with Swift (and also ground-based optical observers).

## 2012ASPC..465..518E - Fighting for Telescope Time? Use the Amateurs!

Eversberg, T.
Abstract: Long-term campaigns, surveys and line monitoring of massive stars can be performed by small telescopes plus adapted spectrographs. Off-the-shelf standard spectrographs are cheap, easy to use and contain respective calibration units. Echelle spectrographs are even delivered with a complete MIDAS-XECHELLE reduction loop. In addition, amateurs design such instrumentation and use it on a professional level. However, the community is small and needs support from the professional side for mutual benefit. Amateurs can deliver design tools, observation time and data. Professionals should deliver scientific knowledge and their organizational skills.
Full text: http://aspbooks.org/custom/publications/paper/465-0518.html

## 2012ASPC..465..372F - 2009: A Colliding-Wind Odyssey

Fahed, R.; Moffat, A. F. J.; Zorec, J.; Eversberg, T.; Chené, A. N.; Alves, F.; Arnold, W.; Bergmann, T.; Corcoran, M. F.; Correia Viegas, N. G.; Dougherty, S. M.; Fernando, A.; Frémat, Y.; Gouveia Carreira, L. F.; Hunger, T.; Knapen, J. H.; Leadbeater, R.; Marques Dias, F.; Martayan, C.; Morel, T.; Pittard, J. M.; Pollock, A. M. T.; Rauw, G.; Reinecke, N.; Ribeiro, J.; Romeo, N.; Sánchez-Gallego, J. R.; dos Santos, E. M.; Schanne, L.; Stahl, O.; Stober, Ba.; Stober, Be.; Vollmann, K.; Williams, P. M.
Abstract: We present the results from two optical spectroscopic campaigns on colliding-wind binaries (CWB) which both occurred in 2009. The first one was on WR 140 (WC7pd + O5.5fc), the archetype of CWB, which experienced periastron passage of its highly elliptical 8-year orbit in January. The WR 140 campaign consisted of a unique and constructive collaboration between amateur and professional astronomers and took place at half a dozen locations, including Teide Observatory, Observatoire de Haute Provence, Dominion Astrophysical Observatory, Observatoire du Mont-Mégantic and at several small private observatories. The second campaign was on a selection of 5 short-period WR + O binaries not yet studied for colliding-wind effects: WR 12 (WN8h), WR 21 (WN5o + O7 V), WR 30 (WC6 + O7.5 V), WR 31 (WN4o + O8), and WR 47 (WN6o + O5). The campaign took place at Leoncito Observatory, Argentina, during 1 month. We provide updated values of most of these systems for the orbital parameters, new estimates for the WR and O star masses and new constraints on the mass-loss rates and colliding wind geometry.
Full text: http://aspbooks.org/custom/publications/paper/465-0372.html

## 2012ASPC..464..235R - Spectroscopic Observations of delta Sco Through the 2011 Periastron Passage

Rivinius, Th.; Stefl, S.; Baade, D.; Carciofi, A. C.; Otero, S.; Miroshnichenko, A. S.; Manset, N.
Abstract: We present prelimiary results from a coordinated spectroscopic campaign in 2011, centered on the delta Sco periastron passage in July. Data have mostly been obtained with the FEROS/2.2 m at La Silla and ESPaDOnS/CFHT at Mauna Kea echelle instruments. Main results include the absence of tidally induced disturbance to the main beta Cephei pulsation mode and the absence of tidally triggered mass-ejection at time of periastron proper. The observed (as far as yet analyzed) variations are compatible with the picture of a disk that is disturbed on its outer radius, with the disturbance propagating inwards after the periastron.
Full text: http://arxiv.org/pdf/1210.0370v1

## 2012ASPC..464..187M - The Be Binary delta Scorpii and Its 2011 Periastron Passage

Miroshnichenko, A. S.; Manset, N.; Pasechnik, A. V.; Carciofi, A. C.; Rivinius, Th.; Stefl, S.; Ribeiro, J. M.; Fernando, A.; Garrel, T.; Knapen, J. H.; Buil, C.; Heathcote, B.; Pollmann, E.; Thizy, O.; Eversberg, T.; Reinecke, N.; Martin, J.; Okazaki, A. T.; Gandet, T. L.; Gvaramadze, V. V.; Zharikov, S. V.
Abstract: delta Scorpii is an unusual Be binary system. The binarity was discovered by interferometry in the 1970's and only confirmed by radial velocity measurements during the periastron passage in September 2000, when the primary component became a Be star. The components brightness and mass suggest that both are normal B-type stars. However, the large orbital eccentricity (e = 0.94) is highly uncommon, as most such Be binaries have circular orbits. The orbital period, only recently constrained by interferometry at 10.81 years, needed confirmation from spectroscopy during the last periastron passage in July 2011. The periastron observing campaign that involved professionals and amateurs resulted in obtaining several hundreds of spectra during the period of a large radial velocity change compared to only thirty obtained in 2000. Along with a determination of the orbital period accurate to 3-4 days, the radial velocity curve was found to be more complicated than one expected from just a binary system. I will briefly review the primary's disk development followed by a discussion of the recent observations. Implications for the system properties and ideas for future observations will be presented.
Full text: http://aspbooks.org/custom/publications/paper/464-0187.html

## 2012ASPC..464...75R - PUCHEROS Early Science: A New Be+sdO Candidate

Rivinius, Th.; Vanzi, L.; Chacon, J.; Leyton, P.; Helminiak., K. G.; Baffico, M.; Stefl, S.; Baade, D.; Avila, G.; Guirao, C.
Abstract: We report on the first scientific results with the recently commissioned PUCHEROS spectrograph, mounted at the 50 cm telescope of the Pontificia Universidad Catolica near Santiago, Chile. A hitherto unknown candidate Be+sdO binary was identified, o Pup. If confirmed, it would be the fourth member of this class. Such stars have obtained their rapid rotation through binary mass transfer and now consist of a Be star and a hot subdwarf.
Full text: http://arxiv.org/pdf/1209.5275v1.pdf

## 2012ApJ...761...99L - A Luminous Be+White Dwarf Supersoft Source in the Wing of the SMC: MAXI J0158-744

Li, K. L.; Kong, Albert K. H.; Charles, P. A.; Lu, Ting-Ni; Bartlett, E. S.; Coe, M. J.; McBride, V.; Rajoelimanana, A.; Udalski, A.; Masetti, N.; Franzen, Thomas
Abstract: We present a multi-wavelength analysis of the very fast X-ray transient MAXI J0158-744, which was detected by MAXI/GSC on 2011 November 11. The subsequent exponential decline of the X-ray flux was followed with Swift observations, all of which revealed spectra with low temperatures (~100 eV), indicating that MAXI J0158-744 is a new Supersoft Source (SSS). The Swift X-ray spectra near maximum show features around 0.8 keV that we interpret as possible absorption from O VIII and emission from O, Fe, and Ne lines. We obtained SAAO and ESO optical spectra of the counterpart early in the outburst and several weeks later. The early spectrum is dominated by strong Balmer and He I emission, together with weaker He II emission. The later spectrum reveals absorption features that indicate a B1/2IIIe spectral type, and all spectral features are at velocities consistent with the Small Magellanic Cloud. At this distance, it is a luminous SSS (>1037 erg s-1) but whose brief peak luminosity of >1039 erg s-1 in the 2-4 keV band makes it the brightest SSS yet seen at "hard" X-rays. We propose that MAXI J0158-744 is a Be-WD binary, and the first example to possibly enter ULX territory. The brief hard X-ray flash could possibly be a result of the interaction of the ejected nova shell with the B star wind in which the white dwarf (WD) is embedded. This makes MAXI J0158-744 only the third Be/WD system in the Magellanic Clouds, but it is by far the most luminous. The properties of MAXI J0158-744 give weight to previous suggestions that SSS in nearby galaxies are associated with early-type stellar systems.
Full text: http://arxiv.org/pdf/1207.5023v3

## 2012AFOEV.142....7T - CI Cygni 2010 Outburst and Eclipse: An Amateur Spectroscopic Survey - First Results From Low Resolution Spectra

Teyssier, F.
Abstract: The aim of this document is to present the amateur spectroscopic survey of the 2010 outburst of symbiotic star CI Cygni by Christian Buil, Thierry Garrel, Benjamin Mauclaire, François Teyssier, Eric Sarrazin, and Pierre Dubreuil (ARAS - Astronomical Ring for Access to Spectroscopy). This outburst coincides with an eclipse of the hot component by the late-type giant star. After a brief review of the current knowledge of this system, the campaign is presented. The first results obtained from low-resolution spectra are described: main emission lines (equivalent width and absolute flux) and continuum evolution in comparison with the CCD V light curve obtained by AAVSO observers.
Full text: http://cdsarc.u-strasbg.fr/afoev/activ/bul/bul-pdf/bullAFOEV142.pdf

## 2012AFOEV.139....4T - Supernova 2011fe

Teyssier, F.; Buil, C.; Thierry, P.; Berardi, P.; Edlin, J.; Garde, O.; Thizy, O.; Desnoux, V.; Garrel, T.
Abstract: Supernova SN2011fe was detected on August 24, 2011. We were able to produce the first intensive long-term spectral follow-up of a supernova made by amateur observers.
Full text: http://cdsarc.u-strasbg.fr/afoev/activ/bul/bul-pdf/bullAFOEV139.pdf

## 2012AAS...21943312B - Long-Term Optical and Near-Infrared Spectroscopic Monitoring of epsilon Aurigae During the 2009-11 Eclipse

Barentine, John C.; Ketzeback, W. F.; Dembicky, J. M.; Huehnerhoff, J.; McMillan, R.; Saurage, G.; Sheldon, A.; Coughlin, J.; Ule, N.; Hawley, S.; Schmidt, S.; Wallerstein, G.; Leadbeater, R.; York, D. G.
Abstract: We present the results of a program to spectroscopically monitor the long-period (P ~ 27 y) eclipsing binary epsilo Aurigae during the primary eclipse of 2009-11 with the ARC 3.5m telescope at Apache Point. Spectroscopic data from 3500-10000Å were obtained at a resolving power of R 38000 and from 0.9-2.5mum at R 3000 with a temporal cadence of approximately one week for the full duration of the eclipse. By noting the velocity centroids of certain weak metal lines (e.g., Na I D and K I 7699Å associated with the presumed optically-thick disk around the unseen secondary, we confirm a mid-eclipse epoch of HJD 2455384. The same lines indicate disk absorption with equivalent widths equal to or greater than the corresponding lines in the primary photosphere. The components of Halpha and their evolution through the eclipse suggest the presence of weak ionized hydrogen, possibly distributed in a circumstellar ring or shell, and a separate, broad ionized component associated with the secondary disk in the form of a disk atmosphere or wind. Overall, our observations support the "consensus model'' of epsilo Aur, consisting of a 2 M&sun;, F0 post-asymptotic giant branch primary and a dust-enshrouded, 6 M&sun; B8 dwarf. Variability of the profiles of certain lines such as Halpha outside of eclipse encourages continued long-term synoptic monitoring of epsilo Aur between primary eclipses to better understand the circumstellar environment of the system.

## 2012A&A...546A..47N - Stochastic gravito-inertial modes discovered by CoRoT in the hot Be star HD 51452

Neiner, C.; Floquet, M.; Samadi, R.; Espinosa Lara, F.; Frémat, Y.; Mathis, S.; Leroy, B.; de Batz, B.; Rainer, M.; Poretti, E.; Mathias, P.; Guarro Fló, J.; Buil, C.; Ribeiro, J.; Alecian, E.; Andrade, L.; Briquet, M.; Diago, P. D.; Emilio, M.; Fabregat, J.; Gutiérrez-Soto, J.; Hubert, A.-M.; Janot-Pacheco, E.; Martayan, C.; Semaan, T.; Suso, J.; Zorec, J.
Abstract: Context. Be stars are rapidly rotating stars with a circumstellar decretion disk. They usually undergo pressure and/or gravity pulsation modes excited by the kappa-mechanism, i.e. an effect of the opacity of iron-peak elements in the envelope of the star. In the Milky Way, p-modes are observed in stars that are hotter than or equal to the B3 spectral type, while g-modes are observed at the B2 spectral type and cooler. Aims: We observed a B0IVe star, HD 51452, with the high-precision, high-cadence photometric CoRoT satellite and high-resolution, ground-based HARPS and SOPHIE spectrographs to study its pulsations in great detail. We also used the lower resolution spectra available in the BeSS database. Methods: We analyzed the CoRoT and spectroscopic data with several methods: Clean-NG, FreqFind, and a sliding window method. We also analyzed spectral quantities, such as the violet over red (V/R) emission variations, to obtain information about the variation in the circumstellar environment. We calculated a stellar structure model with the ESTER code to test the various interpretation of the results. Results: We detect 189 frequencies of variations in the CoRoT light curve in the range between 0 and 4.5 c d-1. The main frequencies are also recovered in the spectroscopic data. In particular we find that HD 51452 undergoes gravito-inertial modes that are not in the domain of those excited by the kappa-mechanism. We propose that these are stochastic modes excited in the convective zones and that at least some of them are a multiplet of r-modes (i.e. subinertial modes mainly driven by the Coriolis acceleration). Stochastically excited gravito-inertial modes had never been observed in any star, and theory predicted that their very low amplitudes would be undetectable even with CoRoT. We suggest that the amplitudes are enhanced in HD 51452 because of the very rapid stellar rotation. In addition, we find that the amplitude variations of these modes are related to the occurrence of minor outbursts. Conclusions: Thanks to CoRoT data, we have detected a new kind of pulsations in HD 51452, which are stochastically excited gravito-inertial modes, probably due to its very rapid rotation. These modes are probably also present in other rapidly rotating hot Be stars. The CoRoT space mission, launched on December 27, 2006, has been developed and is operated by CNES, with the contribution of Austria, Belgium, Brazil, ESA (RSSD, and Science Programs), Germany, and Spain. This work uses observations partly made with the HARPS instrument at the 3.6-m ESO telescope (La Silla, Chile) in the framework of the LP182.D-0356, as well as data obtained with Sophie at OHP and from the BeSS database.Table 3 is available in electronic form at http://www.aanda.org
Full text: http://www.aanda.org/articles/aa/pdf/2012/10/aa19820-12.pdf

## 2012A&A...545A..59S - The relationship between gamma Cassiopeiae's X-ray emission and its circumstellar environment. II. Geometry and kinematics of the disk from MIRC and VEGA instruments on the CHARA Array

Stee, Ph.; Delaa, O.; Monnier, J. D.; Meilland, A.; Perraut, K.; Mourard, D.; Che, X.; Schaefer, G. H.; Pedretti, E.; Smith, M. A.; Lopes de Oliveira, R.; Motch, C.; Henry, G. W.; Richardson, N. D.; Bjorkman, K. S.; Bücke, R.; Pollmann, E.; Zorec, J.; Gies, D. R.; ten Brummelaar, T.; McAlister, H. A.; Turner, N. H.; Sturmann, J.; Sturmann, L.; Ridgway, S. T.
Abstract: Context.gamma Cas is thought to be the prototype of classical Be stars and is the most studied object among this group. However, as for all Be stars, the origin and the physics of its circumstellar disk responsible for the observed near IR-excess, emission lines, and peculiar X-ray emission is still being debated. Aims: We constrain the geometry and kinematics of its circumstellar disk from the highest spatial resolution ever achieved on this star. This investigation is a part of a large multi-technique observing campaign to obtain the most complete picture of gamma Cas which emphasizes the relation of the circumstellar environment to the star's X-ray flux. Methods: We present new observations in the near infrared (MIRC) and in the visible (VEGA) obtained with the CHARA interferometer. The VEGA instrument allows us to not only obtain a global disk geometry but also spectrally dispersed visibility modulus and phases within the Halpha emission line, which enables us to study the kinematics within gamma Cas's disk. Results: We obtain a disk extension in the nearby Halpha continuum of 1.72 stellar diameter and 1.86 stellar diameter in the H band at 1.65 mum assuming a Gaussian disk model but also compatible with an elliptical ring model with a minor internal diameter of 1.38 stellar diameter in H. For the first time we demonstrate that the rotation mapped by the emission in the Halpha line within the disk of gamma Cas and up to 10 R* is Keplerian. Conclusions: These observations have pushed the size of the disk to greater proportions. gamma Cas was also confirmed to be a nearly critical rotator. The disk imaging gives neither indication of a 1-arm spiral feature nor evidence of a secondary star reinforcing the interpretation that the secondary is certainly a low-mass and low-luminosity star or a degenerate companion.
Full text: http://www.aanda.org/articles/aa/pdf/2012/09/aa19234-12.pdf

## 2012A&A...540A..76 - New activity in the large circumstellar disk of the Be-shell star 48 Lib

S. Stefl, J.-B. Le Bouquin, A. C. Carciofi, T. Rivinius, D. Baade, F. Rantakyro
Abstract: Spectroscopic, polarimetric, and high spectral resolution interferometric data covering the period 1995-2011 are analyzed to document the transition into a new phase of circumstellar disk activity in the classical Be-shell star 48 Lib. The long-term disk evolution is described using the V/R ratio of the violet and red emission components of H alpha and Br gamma, radial velocities and profiles of He I and optical metal shell lines, multi-band BVRI polarimetry, broad-band and high-resolution interferometric visibilities and phases. Spectroscopic signatures of disk asymmetries in 48 Lib vanished in the late nineties but recovered some time between 2004 and 2007. Variations in the radial velocity and line profile of conventional shell lines correlate with the V/R behavior. They are shared by narrow absorption cores superimposed on otherwise seemingly photospheric He I lines, which may form in high-density gas at the inner disk close to the photosphere. Large radial velocity variations continued also during the V/R-quiet years. The broad H-band interferometry gives a disk diameter of (1.72+-0.2) mas (equivalent to 15 stellar radii), position angle of the disk (50+-9) deg and a relatively low disk flattening of 1.66+-0.3. Within the errors the same disk position angle is derived from polarimetric observations and from photocenter shifts across Br gamma. The high-resolution interferometric visibility and phase profiles show a double or even multiple-component structure. A preliminary estimate based on the size of the Br gamma emitting region indicates a large diameter for the disk (tens of stellar radii).
Full text: http://arxiv.org/abs/1202.4523v1

## 2012A&A...540A..53S - The relationship between gamma Cassiopeiae's X-ray emission and its circumstellar environment

Smith, M. A.; Lopes de Oliveira, R.; Motch, C.; Henry, G. W.; Richardson, N. D.; Bjorkman, K. S.; Stee, Ph.; Mourard, D.; Monnier, J. D.; Che, X.; Bücke, R.; Pollmann, E.; Gies, D. R.; Schaefer, G. H.; ten Brummelaar, T.; McAlister, H. A.; Turner, N. H.; Sturmann, J.; Sturmann, L.; Ridgway, S. T.
Abstract: gamma Cas is the prototypical classical Be star and is recently best known for its variable hard X-ray emission. To elucidate the reasons for this emission, we mounted a multiwavelength campaign in 2010 centered around four XMM-Newton observations. The observational techniques included long baseline optical interferometry (LBOI) from two instruments at CHARA, photometry carried out by an automated photometric telescope and Halpha observations. Because gamma Cas is also known to be in a binary, we measured radial velocities from the Halpha line and redetermined its period as 203.55 ± 0.20 days and its eccentricity as near zero. The LBOI observations suggest that the star's decretion disk was axisymmetric in 2010, has an system inclination angle near 45°, and a larger radius than previously reported. In addition, the Be star began an "outburst" at the beginning of our campaign, made visible by a brightening and reddening of the disk during our campaign and beyond. Our analyses of the new high resolution spectra disclosed many attributes also found from spectra obtained in 2001 (Chandra) and 2004 (XMM-Newton). As well as a dominant hot ( ˜ 14 keV) thermal component, the familiar attributes included: (i) a fluorescent feature of Fe K even stronger than observed at previous times; (ii) strong lines of N VII and Ne XI lines indicative of overabundances; and (iii) a subsolar Fe abundance from K-shell lines but a solar abundance from L-shell ions. We also found that two absorption columns are required to fit the continuum. While the first one maintained its historical average of 1 × 1021 cm-2, the second was very large and doubled to 7.4 × 1023 cm-2 during our X-ray observations. Although we found no clear relation between this column density and orbital phase, it correlates well with the disk brightening and reddening both in the 2010 and earlier observations. Thus, the inference from this study is that much (perhaps all?) of the X-ray emission from this source originates behind matter ejected by gamma Cas into our line of sight.
Full text: http://arxiv.org/pdf/1201.6415v1

## 2012A&A...537A.148N - Detecting and modelling the magnetic field of the beta Cephei star V 2052 Ophiuchi

Neiner, C.; Alecian, E.; Briquet, M.; Floquet, M.; Frémat, Y.; Martayan, C.; Thizy, O.; Mimes Collaboration
Abstract: Aims: Following the indirect detection of a magnetic field in the beta Cephei star V 2052 Oph by Neiner and collaborators in 2003 with the Musicos spectropolarimeter, we remeasured the magnetic field of this star to attempt to directly confirm the detection of a magnetic field and study its configuration in greater detail. Methods: We used the Narval spectropolarimeter installed at TBL (Pic du Midi, France), which is about 20 times more efficient than the Musicos spectropolarimeter. We applied the least-squares deconvolution (LSD) technique to various groups of lines to measure the circular polarisation of the light coming from V 2052 Oph. We synthesized the measured Stokes V profiles with a centred and off-centred dipole model. Results: For the first time, we clearly detect the Zeeman signature in the Stokes V profiles of V 2052 Oph and thus directly prove the presence of a magnetic field in this star. The modulation with the rotation period is also confirmed and reflects an oblique dipole field. Thanks to the small error bars on the measurements, we are able to study the behaviour of different groups of lines and the centring of the dipole in the star. We find that the dipole is most likely off-centred along the magnetic axis and that He spots are present at the surface next to the magnetic axis. Conclusions: We conclude that V 2052 Oph is a magnetic He-strong beta Cep star, with a dipole field, probably off-centred, with Bpol ~ 400 G and He patches close to the magnetic poles. Based on observations obtained with the Narval spectropolarimeter at the Télescope Bernard Lyot, Observatoire du Pic du Midi, France.
Full text: http://www.aanda.org/articles/aa/pdf/2012/01/aa17941-11.pdf

## 2011MNRAS.418....2F - Spectroscopy of the archetype colliding-wind binary WR 140 during the 2009 January periastron passage

Fahed, R.; Moffat, A. F. J.; Zorec, J.; Eversberg, T.; Chené, A. N.; Alves, F.; Arnold, W.; Bergmann, T.; Corcoran, M. F.; Correia Viegas, N. G.; Dougherty, S. M.; Fernando, A.; Frémat, Y.; Gouveia Carreira, L. F.; Hunger, T.; Knapen, J. H.; Leadbeater, R.; Marques Dias, F.; Martayan, C.; Morel, T.; Pittard, J. M.; Pollock, A. M. T.; Rauw, G.; Reinecke, N.; Ribeiro, J.; Romeo, N.; Sánchez-Gallego, J. R.; Dos Santos, E. M.; Schanne, L.; Stahl, O.; Stober, Ba.; Stober, Be.; Vollmann, K.; Williams, P. M.
Abstract: We present the results from the spectroscopic monitoring of WR 140 (WC7pd + O5.5fc) during its latest periastron passage in 2009 January. The observational campaign consisted of a constructive collaboration between amateur and professional astronomers. It took place at six locations, including Teide Observatory, Observatoire de Haute Provence, Dominion Astrophysical Observatory and Observatoire du Mont Mégantic. WR 140 is known as the archetype of colliding-wind binaries and it has a relatively long period (?8 yr) and high eccentricity (?0.9). We provide updated values for the orbital parameters, new estimates for the WR and O star masses and new constraints on the mass-loss rates and colliding-wind geometry.
Full text: http://mnras.oxfordjournals.org/content/418/1/2.full.pdf+html

## 2011IAUS..272..501F - Spectroscopic follow-up of the colliding-wind binary WR 140 during the 2009 January periastron passage

Fahed, Rémi; Moffat, Anthony F. J.; Zorec, Juan; Eversberg, Thomas; Chené, André-Nicolas; Alves, Filipe; Arnold, Wolfgang; Bergmann, Thomas; Carreira, Luis F. Gouveia; Dias, Filipe Marques; Fernando, Alberto; Gallego, José Sánchez; Hunger, Thomas; Knapen, Johan H.; Leadbeater, Robin; Morel, Thierry; Rauw, Grégor; Reinecke, Norbert; Ribeiro, José; Romeo, Nando; dos Santos, Eva M.; Schanne, Lothar; Stahl, Otmar; Stober, Barbara; Stober, Berthold; Viegas, Nelson G. Correia; Vollmann, Klaus; Corcoran, Michael F.; Dougherty, Sean M.; Pittard, Julian M.; Pollock, Andy M. T.; Williams, Peredur M.
Abstract: We present the results from the spectroscopic follow-up of WR140 (WC7 + O4-5) during its last periastron passage in january 2009. This object is known as the archetype of colliding wind binaries and has a relatively large period (~=8 years) and eccentricity (~=0.89). We provide updated values for the orbital parameters, new estimates for the WR and O star masses and new constraints on the mass-loss rates.
Full text: http://journals.cambridge.org/action/displayAbstract?fromPage=online&aid=8325873&fileId=S1743921311011173

## 2011IAUS..272..414M - Variability monitoring of OB stars during the Mons campaign

Morel, Thierry; Rauw, Gregor; Eversberg, Thomas; Alves, Filipe; Arnold, Wolfgang; Bergmann, Thomas; Viegas, Nelson G. Correia; Fahed, Rémi; Fernando, Alberto; Carreira, Luis F. Gouveia; Hunger, Thomas; Knapen, Johan H.; Leadbeater, Robin; Dias, Filipe Marques; Moffat, Anthony F. J.; Reinecke, Norbert; Ribeiro, José; Romeo, Nando; Gallego, José Sánchez; dos Santos, Eva M.; Schanne, Lothar; Stahl, Otmar; Stober, Barbara; Stober, Berthold; Vollmann, Klaus; Corcoran, Mike F.; Dougherty, Sean M.; Hamaguchi, Kenji; Pittard, Julian M.; Pollock, Andy M. T.; Williams, Peredur M.
Abstract: We present preliminary results of a 4-month campaign carried out in the framework of the Mons project, where time-resolved Halpha observations are used to study the wind and circumstellar properties of a number of OB stars.
Full text: http://arxiv.org/pdf/1009.4627v1

## 2011IAUS..272..282T - Spectrographs for small telescopes

Thizy, Olivier; Cochard, François
Abstract: Shelyak Instruments is a company founded in 2006 offering a full range of spectrographs designed for Astronomy, shipping World Wide. Current users are (1) Public and private observatories who want to setup small telescope for scientific programs or training; (2) Universities for education and demonstrations; (3) Experienced amateurs observers who work in Pro/Amateur collaborations. Lhires III Littrow high resolution spectrograph and eShel optical fibre fed echelle solution are presented with some scientific results including OB stars in which those instruments had a significant contribution.
Full text: http://journals.cambridge.org/action/displayAbstract?fromPage=online&aid=8325697&fileId=S174392131101057X

## 2011IAUS..272..280C - ArasBeam: when amateurs contribute to Be star research

Cochard, François; Desnoux, Valérie; Buil, Christian
Abstract: Since 2003, the amateur astronomical community has decided, in collaboration with the Paris-Meudon Observatory, to coordinate their observations to get the best spectral survey of Be stars as possible. A database for amateur and professional Be star spectra, BeSS, has been created. Spectrographs (up to R=20000) and software tools have been developed for amateurs. Among them, ArasBeam is a web-based tool designed to organize amateur Be spectral observations. A very simple color coding indicates to any observer which stars must be observed on the following night to get the best possible survey of Be stars. So far, more than 11000 amateur spectra have been collected in BeSS. About all bright Be stars (up to magnitude 8) listed in BeSS and visible from the Northern hemisphere have been observed at least one time. In addition, 6 outbursts have been detected by amateurs in the last 2 years.
Full text: http://journals.cambridge.org/action/displayAbstract?fromPage=online&aid=8325695&fileId=S1743921311010568

## 2011epsc.conf..582S - French Pro/Am collaborations in exoplanet

Santerne, A.; Moutou, C.; Vanhuysse, M.; Bouchy, F.; Buil, C.; Cochard, F.; Thizy, O.; Martinez, P.; Desnoux, V.; Pujol, M.; Colas, F.
Abstract: Amateur astronomers have access to huge telescope time and can reach photometric precision up to a few mmag as well as radial velocity precision up to ˜ 50m.s-1 on brightest stars. We will first present some results of french amateur astronomers in transit photometry and radial velocity and then, we will present an over-view of all the collaborations which can be done between professional and amateur astronomers in the competitive exoplanet domain, and especially the current collaboration between french Pro & Am astronomers which was used in publication in A&A. Finally, we will present a new internet wiki page which goal is to develop such collaboration in different countries.
Full text: http://meetings.copernicus.org/epsc-dps2011/

## 2011EAS....47...73D - Spectral data reduction

Desnoux, V.
Abstract: Spectral data reduction is a crucial step, as so important as the acquisition process. Rigor shall be as well applied at this stage to not degrade the quality of the data acquired. It is the last step before the computation of the astrophysical quantities. It is thus necessary to understand what is involved in each processing steps and the underlying limitations. Thus limitations or limit conditions are usually embedded and then hidden in a specific software command that everyone use without completely mastering what is really at stake. In this chapter we will introduced the different type of processing and spectral analysis which can dispose an amateur in several software packages. The first processing will treat about basic images correction which are linked to the CCD acquisition and the processes pipeline. We will then describe the different strategy to calibrate the spectral profile in wavelength and the few corrections driven by the earth environment to increase the accuracy of the future measurements. We will end with the description of few tools on quantitative spectral analysis and their limitations. The practice of spectral acquisition and processing is just at its beginning in amateur world. We hope that this section will demystify the essential step of spectral processing and will motivate the amateur to go beyond the contemplative watching of sky wonders.
Full text: http://www.eas-journal.org/action/displayAbstract?fromPage=online&aid=8459834

## 2011EAS....47...39B - Spectrographs in amateur astronomy

Buil, C.
Abstract: This paper reviews the overall principles of astronomical spectrographs and the design rules that cover low, medium, and high spectral resolution instruments. Several examples of spectrograph designs are described that are easy to build and are optimised for amateur telescopes. Results are given for each of these instruments. Despite the modest size of amateur telescopes, we show that high performance spectrographs in the hands of amateur astronomers provide access to some specialised areas where the amateur could contribute to useful astrophysical work.
Full text: http://www.eas-journal.org/action/displayAbstract?fromPage=online&aid=8459832

## 2011BSRSL..80..668F - Spectroscopic follow-up of the colliding-wind binary WR140 during the 2009 January periastron passage

Fahed, R.; Moffat, A. F. J.; Zorec, J.; Eversberg, T.; Chené, A. N.; Alves, F.; Arnold, W.; Bergmann, T.; Gouveia Carreira, L. F.; Marques Dias, F.; Fernando, A.; Sanchez Gallego, J.; Hunger, T.; Knapen, J.; Leadbeater, R.; Morel, T.; Rauw, G.; Reinecke, N.; Ribeiro, J.; Romeo, N.; Dos Santos, E. M.; Schanne, L.; Stahl, O.; Stober, Ba.; Stober, Be.; Correia Viegas, N. G.; Vollmann, K.; Corcoran, M. F.; Dougherty, S. M.; Pittard, J. M.; Pollock, A. M. T.; Williams, P. M.
Abstract: We present the results from the spectroscopic follow-up of WR140 (WC7 + O4-5) during its last periastron passage in January 2009. This object is known as the archetype of colliding wind binaries and has a relatively large period (~=8 years) and eccentricity (~=0.9). We provide updated values for the orbital parameters, new estimates for the WR and O star masses and new constraints on the mass-loss rates.
Full text: http://popups.ulg.ac.be/0037-9565/index.php?id=3137&file=1&pid=3133

## 2011BSRSL..80..469E - Spectroscopic madness - A golden age for amateurs

Eversberg, Thomas
Abstract: Today, professional instrumentation is dominated by heavily oversubscribed telescopes which focus mainly on a limited number of fashionable'' research topics. As a result, time acquisition for massive star research including extended observation campaigns, becomes more difficult. On the other hand, massive star investigations by amateur astronomers performing spectroscopic measurements are on a level which can fulfil professional needs. I describe the instrumentation available to the amateurs, their observational skills and the potential contribution they can make to the professional community.
Full text: http://popups.ulg.ac.be/0037-9565/index.php?id=2966&file=1&pid=2964

## 2011BSRSL..80..170M - The Mons campaign on OB stars

Morel, T.; Rauw, G.; Eversberg, T.; Alves, F.; Arnold, W.; Bergmann, T.; Correia Viegas, N. G.; Fahed, R.; Fernando, A.; Gouveia Carreira, L. F.; Hunger, T.; Knapen, J. H.; Leadbeater, R.; Marques Dias, F.; Moffat, A. F. J.; Reinecke, N.; Ribeiro, J.; Romeo, N.; Sánchez Gallego, J.; Dos Santos, E. M.; Schanne, L.; Stahl, O.; Stober, Ba.; Stober, Be.; Vollmann, K.; Corcoran, M. F.; Dougherty, S. M.; Hamaguchi, K.; Pittard, J. M.; Pollock, A. M. T.; Williams, P. M.
Abstract: In parallel with the monitoring of the periastron passage of the binary system WR 140, a number of B supergiants and Oe stars have been observed in the framework of a 4-month spectroscopic run using the Mons telescope at Teide observatory. We expose the motivations behind this campaign, present an overview of the Halpha variations exhibited by the B supergiants and finally briefly discuss forthcoming developments in the data analysis.
Full text: http://popups.ulg.ac.be/0037-9565/index.php?id=2658&file=1&pid=2626

## 2011BAVSR..60..229H - VV Cep - helligkeitsmessungen mit einer digitalkamera und spektroskopisches halpha-monitoring.

Hassforther, B.; Pollmann, E.

## 2011BAVSR..60...87P - Die beobachtungskampagne der Delta-Scorpii - periastron-passage 2011.

Pollmann, E.; Miroshnichenko, A.

Pollmann, E.

## 2011AJ....142..149N - The Be Star Spectra (BeSS) Database

Neiner, C.; de Batz, B.; Cochard, F.; Floquet, M.; Mekkas, A.; Desnoux, V.
Abstract: Be stars vary on many timescales, from hours to decades. A long time base of observations to analyze certain phenomena in these stars is therefore necessary. Collecting all existing and future Be star spectra into one database has thus emerged as an important tool for the Be star community. Moreover, for statistical studies, it is useful to have centralized information on all known Be stars via an up-to-date catalog. These two goals are what the Be Star Spectra (BeSS, http://basebe.obspm.fr) database proposes to achieve. The database contains an as-complete-as-possible catalog of known Be stars with stellar parameters, as well as spectra of Be stars from all origins (any wavelength, any epoch, any resolution, etc.). It currently contains over 54,000 spectra of more than 600 different Be stars among the ~2000 Be stars in the catalog. A user can access and query this database to retrieve information on Be stars or spectra. Registered members can also upload spectra to enrich the database. Spectra obtained by professional as well as amateur astronomers are individually validated in terms of format and science before being included in BeSS. In this paper, we present the database itself as well as examples of the use of BeSS data in terms of statistics and the study of individual stars.
Full text: http://iopscience.iop.org/1538-3881/142/5/149/pdf/aj_142_5_149.pdf

## 2011AAS...21743104F - RSpec: New Real-time Spectroscopy Software Enhances High School and College Learning

Field, Tom
Abstract: Nothing beats hands-on experience! Students often have a more profound learning experience in a hands-on laboratory than in a classroom. However, development of inquiry-based curricula for teaching spectroscopy has been thwarted by the absence of affordable equipment. There is now a software program that brings the excitement of real-time spectroscopy into the lab. It eliminates the processing delays that accompany conventional after-the-fact data analysis -- delays that often result in sagging enthusiasm and loss of interest in young, active minds. RSpec is the ideal software for high school or undergraduate physics classes. It is a state-of-the-art, multi-threaded software program that allows students to observe spectral profile graphs and their colorful synthesized spectra in real-time video. Using an off-the-shelf webcam, DSLR, cooled-CCD or even a cell phone camera, students can now gain hands-on experience in gathering, calibrating, and identifying spectra. Light sources can include the sun, bright night-time astronomical objects, or gas tubes. Students can even build their own spectroscopes using inexpensive diffraction "rainbow'' glasses. For more advanced students, the addition of an inexpensive slitless diffraction grating allows the study of even more exciting objects. With a modest 8'' telescope, students can use a simple webcam to classify star types, and to detect such exciting phenomena as Neptune's methane-absorption lines, M42's emission lines, and even, believe it or not, the redshift of 3C 273. These adventures are possible even under light-polluted urban skies. RSpec is also an excellent program for amateur astronomers who want to transition from visual CCD imaging to actual scientific data collection and analysis. As the developer of this software, I worked with both teachers and experienced spectroscopists to ensure that it would bring a compelling experience to your students. The response to real-time, colorful data has been very enthusiastic both in the classroom and in public outreach.

## 2011AAS...21733924M - The Delta Scorpii Be Binary. The Disk Development and Periastron 2011.

Miroshnichenko, Anatoly S.; Stefl, S.; Manset, N.; Bjorkman, K. S.; Korpela, M.; Davidson, J.; Rivinius, T.; Okazaki, A. T.; Carciofi, A. C.; Pollmann, E.; Heathcote, B.; Levato, H.; Grosso, M.; Fabregat, J.; Zharikov, S. V.
Abstract: Delta Scorpii is a bright (V=2.3 mag) binary system with a B0-type primary and supposedly a B-type secondary at an eccentric orbit (e=0.94). A brightening detected in the summer of 2000 marked the beginning of a circumstellar disk formation around the primary component. It occurred a few months before the periastron which was detected through a strong radial velocity change in September 2000. We present a history of the disk development and discuss possible explanations for the observed variations of the optical and near-infrared brightness and emission line profiles. The next periastron is predicted to occur in early July 2011. We emphasize the importance of frequent observations of Delta Scorpii with various techniques in 2011, predict some phenomena that may occur near periastron, and suggest observing strategies.

## 2011AAS...21725705K - Optical and NIR Spectroscopy of e Aurigae at Apache Point Observatory, the First Half of the Eclipse

Ketzeback, William F.; Barentine, J.; Leadbeater, R.; McMillan, R.; Dembicky, J.; Saurage, G.; Huehnerhoff, J.; Schmidt, S.; Hawley, S.; Wallerstein, G.; Coughlin, J.; York, D.
Abstract: Epsilon Aurigae (e Aur), first confirmed as a variable in 1821, is an eclipsing binary star system with a period of 27.1 years, one of the longest known. The primary, a pulsating F supergiant star with a variability out of eclipse of approximately 60 days and possible overtones of hundreds of days, is orbited by the secondary, a B-star enveloped by an enormous, cool, spectrally gray disk producing no evident wavelength dependence to the light output variations. The eclipse lasts for over 700 days; the current eclipse began first contact in July, 2009, and August 4, 2010 marked the estimated midway point of the eclipse. Although the components of the system have now been identified, much is still unclear such as the origin, composition and structure of the disk. Modern digital spectroscopy of bright stars not only enables asteroseismology and planetary detection, but the eclipsing binary epsilon Aurigae is an unusual case in which precise spectroscopic study of the now transiting dark disk is enabled. At Apache Point Observatory, our team has conducted high-resolution optical and NIR spectroscopic monitoring of this mysterious eclipsing system since February, 2009. We present major changes in the spectra attributable to the disk from the first half of the eclipse in the 0.4 - 2.2 mum range using ARCES, an optical echelle spectrograph (lambda/Deltalambda=31,500), and Triplespec, a NIR cross-dispersed spectrograph (lambda/Deltalambda=3500), on the ARC 3.5-meter telescope.

## 2011AAS...21725704L - Spectroscopic Wonders During The 2010 Eclipse Of Epsilon Aurigae

Leadbeater, Robin; Buil, C.; Garrell, T.; Gorodenski, S.; Hopkins, J.; Mauclaire, B.; Ribeiro, J.; Schanne, L.; Thizy, O.; Stencel, R.
Abstract: Remarkable spectroscopic coverage is reported of the 2009-2011 eclipse of the enigmatic binary, epsilon Aurigae. Due to the availability of new spectrographs and digital detectors, unprecedented monitoring by a network of observers using small telescopes has revealed a number of details and surprises that must be taken into account in any updated model for the over-luminous F star and the dark disk companion, recently detected interferometrically. Over 400 spectra were obtained during 2007 to 2010 (pre eclipse to post mid eclipse). They include R 12000 echelle spectra giving broad coverage from 4300-7000A and detailed spectra at R 17000-25000 covering the Sodium D, Hydrogen alpha and Potassium 7699A line regions. Evidence of the eclipsing body was first seen in the 7699A line profile 83 days before photometric first contact. During ingress, the strength of this line increased in a stepwise fashion suggesting structure in the disc. During the first half of totality, the line strength trend deviated from that seen during the last eclipse. Radial velocity measurements of the 7699A line during ingress are consistent with the disc material orbiting a central object of 5.3 solar masses. Changes in the Hydrogen alpha line profile during totality reveal the presence of a foreground emission source centered at the systemic radial velocity. A small transient emission line has been seen at 6604A on two occasions during the eclipse. This work was supported in part by the bequest of William Herschel Womble in support of astronomy at the University of Denver, and by NSF grant 1016678 to the University of Denver. We are grateful for the assistance of the epsilon Aurigae spectral monitoring team at Apache Point Observatory (W. Ketzeback, J.Barentine, et al.) and all observers participating in the international eclipse monitoring campaign.

## 2010SASS...29...13H - Epsilon Aurigae Eclipse 2009 – Ingress

Hopkins, Jeffrey L.; Stencel, Robert E.; Leadbeater, Robin; Beckmann, Paul J.; Buil, Christian; Collins, Donald; Colombo, Tiziano; Garrel, Thierry; Gorodenski, Stanley; Gudmundsson, Snaevarr; Karlsson, Mukund Kurtadikar; Lindberg, Hans-Goran; Loughney, Des; Mauclaire, Benji; McCandless, Brian E.; Melillo, Frank J.; Miles, Richard; Pearson, Robert T.; Samolyk, Gerard; Schanne, Lothar; Strikis, Iakovos Marios; Teyssier, François; Thizy, Olivier
Abstract: The mysterious star system epsilon Aurigae undergoes an eclipse every 27.1 years that lasts nearly two years. The most recent eclipse started during the late summer of 2009. An international campaign for observing this eclipse was created in 2006, with a web site for information and, to-date, 17 periodic newsletters for details, as well as a Yahoo forum List for immediate announcements and comments. Photometric data in the UBVRIJH bands have been submitted. Ingress occurred with first contact in the V band estimated at the second week of 2009 August and second contact estimated at 2010 mid-January. Spectroscopic data were also obtained during ingress. Spectroscopic data have been provided in the potassium I region, hydrogen alpha and beta regions and sodium D line region of the star system's spectrum. In this paper we describe details of observations and preliminary analysis during ingress and second contact. We introduce the observers and discuss plans for observing throughout totality and the end of the eclipse in 2011.

Ribeiro, José

Pollmann, E.

## 2010BAVSR..59..155B - Radialgeschwindigkeitsmessungen an der HeI6678-Linie am be-doppelstern zeta Tau.

Buecke, R.; Pollmann, E.

## 2010BAVSR..59...15P - H-alpha-Beobachtungen am Doppelsternsystem Zeta Tau

Pollmann, Ernst; Rivinius, Th.
Abstract: Longtime-observations and their interpretation on Zeta Tau in H-alpha are shown.

## 2010AAS...21541935K - An Unusual Interacting Eclipsing Binary

Kelley, Joshua; Gray, R.; Mais, D.; Caton, D.; Smith, A.
Abstract: HD5501 is an unusual eclipsing binary star discovered in the course of a survey for classical A-type shell stars. It initially excited interest because it shows variable shell lines. We report here on photometry and spectroscopy of this star carried out over a number of years. We derive the orbital period,estimate the mass of its primary star, and deduce the existence of an accretion disk around the secondary which appears to be a compact object.

## 2010A&A...521A...5C - Time, spatial, and spectral resolution of the Halpha line-formation region of Deneb and Rigel with the VEGA/CHARA interferometer

Chesneau, O.; Dessart, L.; Mourard, D.; Bério, Ph.; Buil, Ch.; Bonneau, D.; Borges Fernandes, M.; Clausse, J. M.; Delaa, O.; Marcotto, A.; Meilland, A.; Millour, F.; Nardetto, N.; Perraut, K.; Roussel, A.; Spang, A.; Stee, P.; Tallon-Bosc, I.; McAlister, H.; ten Brummelaar, T.; Sturmann, J.; Sturmann, L.; Turner, N.; Farrington, C.; Goldfinger, P. J.
Abstract: Context. BA-type supergiants are amongst the most optically-bright stars. They are observable in extragalactic environments, hence potential accurate distance indicators. Aims: An extensive record of emission activity in the Halpha line of the BA supergiants beta Orionis (Rigel, B8Ia) and alpha Cygni (Deneb, A2Ia) is indicative of localized time-dependent mass ejections. However, little is known about the spatial distribution of these apparent structures. Here, we employ optical interferometry to study the Halpha line-formation region in these stellar environments. Methods: High spatial- ( 0.001'') and spectral- (R = 30 000) resolution observations of Halpha were obtained with the visible recombiner VEGA installed on the CHARA interferometer, using the S1S2 array-baseline (34 m). Six independent observations were done on Deneb during the years 2008 and 2009, and two of Rigel in 2009. We analyze this dataset with the 1D non-LTE radiative-transfer code cmfgen, and assess the impact of the wind on the visible and near-IR interferometric signatures, using both Balmer-line and continuum photons. Results: We observe a visibility decrease in Halpha for both Rigel and Deneb, suggesting that the line-formation region is extended ( 1.5-1.75 Rstar). We observe a significant visibility decrease for Deneb in the Siii 6371 Å line. We witness time variations in the differential phase for Deneb, implying an inhomogeneous and unsteady circumstellar environment, while no such variability is seen in differential visibilities. Radiative-transfer modeling of Deneb, with allowance for stellar-wind mass loss, accounts fairly well for the observed decrease in the Halpha visibility. Based on the observed differential visibilities, we estimate that the mass-loss rate of Deneb has changed by less than 5%.
Full text: http://arxiv.org/pdf/1007.2095v1

## 2010A&A...516A..80N - Properties and nature of Be stars. 27. Orbital and recent long-term variations of the Pleiades Be star Pleione = BU Tauri

Nemravová, J.; Harmanec, P.; Kubát, J.; Koubský, P.; Iliev, L.; Yang, S.; Ribeiro, J.; Slechta, M.; Kotková, L.; Wolf, M.; Skoda, P.
Abstract: Radial-velocity variations of the Halpha emission measured on the steep wings of the Halpha line, prewhitened for the long-time changes, vary periodically with a period of 218.025 ° ± 0.022°, confirming the suspected binary nature of the bright Be star BU Tau, a member of the Pleiades cluster. The orbit seems to have a high eccentricity over 0.7, but we also briefly discuss the possibility that the true orbit is circular and that the eccentricity is spurious owing to the phase-dependent effects of the circumstellar matter. The projected angular separation of the spectroscopic orbit is large enough to allow the detection of the binary with large optical interferometers, provided the magnitude difference primary - secondary is not too large. Since our data cover the onset of a new shell phase up to development of a metallic shell spectrum, we also briefly discuss the recent long-term changes. We confirm the formation of a new envelope, coexisting with the previous one, at the onset of the new shell phase. We find that the full width at half maximum of the Halpha profile has been decreasing with time for both envelopes. In this connection, we briefly discuss Hirata's hypothesis of precessing gaseous disk and possible alternative scenarios of the observed long-term changes. Based on new spectral and photometric observations from the following observatories: Dominion Astrophysical Observatory, Herzberg Institute of Astrophysics, National Research Council of Canada, Haute Provence, IGeoE-Lisbon, Astronomical Institute AS CR Ondrejov, and Rozhen.
Full text: http://www.aanda.org/articles/aa/pdf/2010/08/aa13885-09.pdf

## 2009MNRAS.398.1505S - On the incidence of magnetic fields in slowly pulsating B, beta Cephei and B-type emission-line stars

Silvester, J.; Neiner, C.; Henrichs, H. F.; Wade, G. A.; Petit, V.; Alecian, E.; Huat, A.-L.; Martayan, C.; Power, J.; Thizy, O.
Abstract: We have obtained 40 high-resolution circular spectropolarimetric measurements of 12 slowly pulsating B (SPB) stars, eight beta Cephei stars and two Be stars with the Echelle Spectropolarimetric Device for the Observation of Stars at CFHT (ESPaDOnS) and Narval spectropolarimeters. The aim of these observations is to evaluate recent claims of a high incidence of magnetic field detections in stars of these types obtained using low-resolution spectropolarimetry by Hubrig et al. The precision achieved is generally comparable to or superior to that obtained by Hubrig et al., although our new observations are distinguished by their resolution of metallic and He line profiles, and their consequent sensitivity to magnetic fields of zero net longitudinal component. In the SPB stars, we confirm the detection of magnetic field in one star (16 Peg), but find no evidence of the presence of fields in the remaining 11. In the beta Cep stars, we detect a field in xi1 CMa, but not in any of the remaining seven stars. Finally, neither of the two B-type emission-line stars shows any evidence of magnetic field. Based on our results, we conclude that fields are not common in SPB, beta Cep and B-type emission-line stars, consistent with the general rarity of fields in the broader population of main sequence B-type stars. A relatively small, systematic underestimation of the error bars associated with the UV Focal Reducer and Low Dispersion Spectrograph for the Very Large Telescope (FORS1) longitudinal field measurements of Hubrig et al. could in large part explain the discrepancy between their results and those presented here.
Full text: http://mnras.oxfordjournals.org/content/398/3/1505.full.pdf+html

Thizy, O.

## 2009IAUS..259..393H - The magnetic field of the B3V star 16 Pegasi

Henrichs, Huib F.; Neiner, C.; Schnerr, R. S.; Verdugo, E.; Alecian, A.; Catala, C.; Cochard, F.; Gutiérrez, J.; Huat, A.-L.; Silvester, J.; Thizy, O.
Abstract: The slowly pulsating B3V star 16 Pegasi was discovered by Hubrig et al. (2006) to be magnetic, based on low-resolution spectropolarimetric observations with FORS1 at the VLT. We have confirmed the presence of a magnetic field with new measurements with the spectropolarimeters Narval at TBL, France and Espadons at CFHT, Hawaii during 2007. The most likely period is about 1.44 d for the modulation of the field, but this could not be firmly established with the available data set. No variability has been found in the UV stellar wind lines. Although the star was reported once to show Halpha in emission, there exists at present no confirmation that the star is a Be star.

## 2009CBET.1885....1W - Epsilon Aurigae

Waagen, E. O.; Leadbeater, R.; Rzepka, M.; Abbott, P.; Makela, V.; Baroni, S.; Maurer, P.; McCandless, B.; Rutherford, T.; Samolyk, G.; Miles, R.
Abstract: E. O. Waagen, AAVSO, writes that R. Leadbeater, Wigton, U.K., reported (via the AAVSO Discussion Group) the spectroscopic detection of the start of a predicted eclipse for the long-period binary star epsilon Aur. The last eclipse was in 1982-1984...
Full text: http://www.cbat.eps.harvard.edu/iau/cbet/001800/CBET001885.txt

## 2009BAVSR..58..236P - Helligkeitsmessungen in V und H-alpha-Spektroskopie am be-stern gamma Cas.

Pollmann, E.; Puscas, F.

Pollmann, E.

## 2009A&A...506..143N - The pulsations of the B5IVe star HD 181231 observed with CoRoT and ground-based spectroscopy

Neiner, C.; Gutiérrez-Soto, J.; Baudin, F.; de Batz, B.; Frémat, Y.; Huat, A. L.; Floquet, M.; Hubert, A.-M.; Leroy, B.; Diago, P. D.; Poretti, E.; Carrier, F.; Rainer, M.; Catala, C.; Thizy, O.; Buil, C.; Ribeiro, J.; Andrade, L.; Emilio, M.; Espinosa Lara, F.; Fabregat, J.; Janot-Pacheco, E.; Martayan, C.; Semaan, T.; Suso, J.; Baglin, A.; Michel, E.; Samadi, R.
Abstract: Context: HD 181231 is a B5IVe star, which has been observed with the CoRoT satellite during ~5 consecutive months and simultaneously from the ground in spectroscopy and spectropolarimetry. Aims: By analysing these data, we aim to detect and characterize as many pulsation frequencies as possible, to search for the presence of beating effects possibly at the origin of the Be phenomenon. Our results will also provide a basis for seismic modelling. Methods: The fundamental parameters of the star are determined from spectral fitting and from the study of the circumstellar emission. The CoRoT photometric data and ground-based spectroscopy are analysed using several Fourier techniques: Clean-ng, Pasper, and Tisaft, as well as a time-frequency technique. A search for a magnetic field is performed by applying the LSD technique to the spectropolarimetric data. Results: We find that HD 181231 is a B5IVe star seen with an inclination of ~45 degrees. No magnetic field is detected in its photosphere. We detect at least 10 independent significant frequencies of variations among the 54 detected frequencies, interpreted in terms of non-radial pulsation modes and rotation. Two longer-term variations are also detected: one at ~14 days resulting from a beating effect between the two main frequencies of short-term variations, the other at ~116 days due either to a beating of frequencies or to a zonal pulsation mode. Conclusions: Our analysis of the CoRoT light curve and ground-based spectroscopic data of HD 181231 has led to the determination of the fundamental and pulsational parameters of the star, including beating effects. This will allow a precise seismic modelling of this star. Based on observations obtained with the CoRoT satellite, with FEROS at the 2.2 m télescope of the La Silla Observatory under the ESO Large Programme LP178.D-0361, with Narval at the Télescope Bernard Lyot of the Pic du Midi Observatory, and collected from the BeSS database. Table 5 is only available in electronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/506/143
Full text: http://www.aanda.org/articles/aa/pdf/2009/40/aa11971-09.pdf

## 2009A&A...504..929S - Cyclic variability of the circumstellar disk of the Be star zeta Tau

Stefl, S.; Rivinius, Th.; Carciofi, A. C.; Le Bouquin, J.-B.; Baade, D.; Bjorkman, K. S.; Hesselbach, E.; Hummel, C. A.; Okazaki, A. T.; Pollmann, E.; Rantakyrö, F.; Wisniewski, J. P.
Abstract: Context: Emission lines formed in decretion disks of Be stars often undergo long-term cyclic variations, especially in the violet-to-red (V/R) ratio of their primary components. The underlying structural and dynamical variations of the disks are only partly understood. From observations of the bright Be-shell star zeta Tau, the possibly broadest and longest data set illustrating the prototype of this behaviour was compiled from our own and archival observations. It comprises optical and infrared spectra, broad-band polarimetry, and interferometric observations. Aims: The dense, long-time monitoring permits a better separation of repetitive and ephemeral variations. The broad wavelength coverage includes lines formed under different physical conditions, i.e. different locations in the disk, so that the dynamics can be probed throughout much of the disk. Polarimetry and interferometry constrain the spatial structure. All together, the objective is a better understand the dynamics and life cycle of decretion disks. Methods: Standard methods of data acquisition, reduction, and analysis were applied. Results: From 3 V/R cycles between 1997 and 2008, a mean cycle length in Halpha of 1400-1430 days was derived. After each minimum in V/R, the shell absorption weakens and splits into two components, leading to 3 emission peaks. This phase may make the strongest contribution to the variability in cycle length. There is no obvious connection between the V/R cycle and the 133-day orbital period of the not otherwise detected companion. V/R curves of different lines are shifted in phase. Lines formed on average closer to the central star are ahead of the others. The shell absorption lines fall into 2 categories differing in line width, ionization/excitation potential, and variability of the equivalent width. They seem to form in separate regions of the disk, probably crossing the line of sight at different times. The interferometry has resolved the continuum and the line emission in Brgamma and HeI 2.06. The phasing of the Brgamma emission shows that the photocenter of the line-emitting region lies within the plane of the disk but is offset from the continuum source. The plane of the disk is constant throughout the observed V/R cycles. The observations lay the foundation for the fully self-consistent, one-armed, disk-oscillation model developed in Paper II. Based partly on observations collected at the European Southern Observatory, Chile (Prop. Nos. 073.D-0234, 074.D-0240, 078.D-0542, and 081.D-2005; as well as archival data from programs 074.D-0573 and 076.B-0055).
Full text: http://arxiv.org/pdf/0907.2250v1

## 2008SASS...27...49T - Classical Be Stars High Resolution Spectroscopy

Thizy, Olivier
Abstract: Classical Be stars are non-giant B-type stars that exhibit or have exhibited emission lines over the photospheric spectrum. The author will review common knowledge of Be stars, a study on Beta Lyr binary Be star, what can be achieved today with commercially available high resolution Lhires III spectrograph, the status of a Be Star Spectra pro/am database, and professional/amateur astronomer collaborations in several countries.

## 2008P&SS...56.1878T - Organizing a professional amateur collaboration with a Lhires III spectrograph

Thizy, Olivier; Buil, Christian; Cochard, François; Neiner, Coralie
Abstract: Amateur spectroscopists are getting organized to contribute to professional astronomy work. We present here the work done within the AUDE association to design, manufacture and distribute the Lhires III high-resolution Littrow spectrograph, which fits usual amateur telescopes and CCD cameras. We also review how the communication is organized through the ARAS distribution list (Spectro-L), forums, and workshops to develop and promote spectroscopic work among amateurs. Last but not least, we introduce the Be stars spectra (BeSS) Virtual Observatory-compatible database and its use for the monitoring of Be stars in association with the COROT satellite.
Full text: http://www.sciencedirect.com/science/article/pii/S0032063308001943

## 2008IBVS.5813....1P - Halpha observations of zeta Tauri.

Pollmann, E.; Rivinius, T.
Abstract: We report H-alpha observations of zeta Tauri, taken between late 2000 and early 2006. Next to extending existing long-term montioring of the disk state of this star we report an intermediate timescale of about 69 days to be present in the V/R variations of the Halpha line. The observational data will be published together with this manuscript.
Full text: http://arxiv.org/pdf/0801.4530v1

## 2008ASPC..401..227S - Non-spherical Mass Outflow from RS~Ophiuchi During its 2006 Outburst

Skopal, A.; Pribulla, T.; Buil, Ch.; Vittone, A.; Errico, L.
Abstract: We present results of our modeling the of Halpha line profile during the 2006 outburst of RS Oph. At day 1.38 it was possible to fit the very broad component of the Halpha by a bipolar wind model. The model corresponds to a very fast acceleration of the wind particles, and the line luminosity of ˜ 2 900 (d/1.6 kpc)^2 L_{&sun;}, to a mass-loss rate of ˜ (1-2)× 10^{-4}myr. During days 10-30 the broad component shrank to FWZI ˜ 1 800 km s^{-1}. It could be associated with expanding ring and its satellite components at ˜± 2 430 km s^{-1} with bipolar jets. Later observations made at day 57 and 209 indicated a decrease in both the mass-loss rate (˜ 1× 10^{-5} - 1× 10^{-6}myr) and the wind acceleration. During the quiet phase, emission bumps observed sporadically in the line wings could reflect clumpy ejections by the central star.
Full text: http://arxiv.org/pdf/0802.3711v1.pdf

## 2007SASS...26...31T - Lhires III High Resolution Spectrograph

Thizy, O.
Abstract: By spreading the light from celestial objects by wavelength, spectroscopists are like detectives looking for clues and identifying guilty phenomena that shape their spectra. We will review some basic principles in spectroscopy that will help, at our amateur level, to understand how spectra are shaped. We will review the Lhires III highresolution spectrograph Mark Three that was designed to reveal line profile details and subtle changes. Then, we will do an overview of educational and scientific projects that are conducted with the Lhires III and detail the COROT Be star program and the BeSS database for which the spectrograph is a key instrument.

Pollmann, E.

## 2007IAUC.8862....2B - Nova Vulpeculae 2007

Buil, C.; Fujii, M.
Abstract: C. Buil, Castanet, France, writes that a spectrogram of the possible nova reported on IAUC 8861, obtained on Aug. 9.91 UT with a 0.28-m telescope (+ Lhires spectrograph; resolution 6800 at H_alpha), shows evident H_alpha with a deep P-Cyg profile and a FWHM of 1750 km/s (+/- 80 km/s); the intensity of the H_alpha peak intensity is 2.4 times that of the local 670-nm continuum...
Full text: http://www.cbat.eps.harvard.edu/iauc/08800/08862.html#Item2

## 2007IAUC.8812....4B - V1280 Scorpii

Buil, C.; West, J. D.
Abstract: C. Buil, Castanet, France, reports that an optical spectrogram of V1280 Sco obtained on Feb. 20.20 UT using a 0.28-m Schmidt- Cassegrain telescope (+ Lhires spectrograph) shows an H_alpha P-Cyg profile and a FWHM of 730 km/s; the intensity of the H_alpha peak intensity is 2.3 times the local 670-nm continuum...
Full text: http://www.cbat.eps.harvard.edu/iauc/08800/08812.html#Item4

## 2007CBET..894....3B - Nova Cygni 2007

Buil, C.

Full text: http://www.cbat.eps.harvard.edu/iau/cbet/000800/CBET000894.txt

## 2007BeSN...38....8P - Possible He I 6678 Emission Activity in gamma Cas

Pollmann, Ernst; Stober, Berthold

Full text: http://www.konkoly.hu/cgi-bin/IBVSpdf?5778

## 2006CBET..403....1B - RS Ophiuchi

Buil, C.

Full text: http://www.cbat.eps.harvard.edu/iau/cbet/000400/CBET000403.txt

## 2005SASS...24..129D - Spectroscopic Monitoring of Be type Stars

Desnoux, V.; Buil, C.
Abstract: The study of Be stars is a perfect example of spectrography that amateurs can participate in. Several types of spectroscopes can be used depending of what physical parameters are monitored: classical surveys at low-resolution or high-resolution profile study of the H-alpha line are just two examples of what can be monitored. By grouping observations on long time scales, a database of stellar spectra can be built and placed at the disposal of professionals. Over a period of 10 years, starting at the Pic du Midi observ- atory and continuing later on by Christian Buil, and other French amateur groups using Musicos professional spectroscope, the monitoring of Be stars produced scientific results and are now supported by professional astron- omers. Some are already using the ARAS (Astronomical Ring for Amateur Spec- troscopy) list to ask for specific monitoring and get additional observations from the amateur community. Spectral processing will be also discussed, using Visual Spec and Iris freeware, from the basic calibration up to time reso- lution H-alpha profile evolution and Equivalent Width computation. Be Stars survey is just an example of how powerful spectroscopy can be, and can be practiced by amateurs. Amateurs are really capable of playing a key part in astrophysical studies.

## 2005PASP..117..938M - Spectra and Light Curve Analysis of Nova V475 Scuti

Morgan, G. E.; Ringwald, F. A.; Buil, C.; Garrett, M.
Abstract: This paper collects together early IAU Circular observations, plots the light curve, and presents our own spectra of V475 Scuti (Nova Sct 2003). We describe the early spectral evolution of this nova during the 7 weeks after its discovery. The principal spectra show this nova to be a common Fe II type (R. E. Williams et al.). The nova displayed dominant Balmer lines and numerous Fe II multiplets (42, 48, 49, 55, and 74), with strong, well-distributed P Cygni profiles that disappeared near the end of our observations. Spectral evolution produced low-ionization forbidden lines consistent with an auroral phase (R. E. Williams et al.). V475 Sct was a fast nova, with t2=22 days and with a type Ba light curve (H. W. Duerbeck) from the American Association of Variable Star Observers. The Halpha velocity widths showed a twofold increase, together with an unusual broadening of the line, during our observations. The lack of structure within the high-resolution Halpha profiles suggests that the nova is exhibiting an isotropic expansion as an optically thick wind, which may result in material falling back onto the white dwarf. We encourage further monitoring.
Full text: http://www.jstor.org/stable/pdfplus/10.1086/432227.pdf

## 2005PAICz..93...44P - Observations of H-alpha Emission in VV Cephei

Pollmann, E.
Abstract: Spectroscopic H-alpha observations during the recent eclipse of the long-periodic M2Iab+B binary VV Cephei are reported. Next to the delay of mid-eclipse with respect to the published ephemeris, an increase of the line emission after the event is reported.

## 2005PAICz..93...14P - Amateur Spectroscopy of Hot Stars. Long term tracking of circumstellar emission

Pollmann, E.
Abstract: The spectroscopic monitoring programs carried out by the Spectroscopy Group of the German Vereinigung der Sternfreunde'' are reviewed in light of current research. Potential benefits for the professional community in collaborating and obtain long-term monitoring data otherwise unaccessible due to telescope time restrictions are summarized. The contribution highlights results on specific objects of wide interest, such as the well investigated Be stars zeta Tauri or the S Doradus type variable P Cygni.

Mais, Dale E.

Pollmann, E.

## 2005A&A...437..257N - Rotation, pulsations and outbursts in the Be star upsilo Cygni (HD 202904)

Neiner, C.; Floquet, M.; Hubert, A. M.; Frémat, Y.; Hirata, R.; Masuda, S.; Gies, D.; Buil, C.; Martayan, C.
Abstract: upsilon Cyg is a Be star that shows variations at all timescales. We monitored its spectrum for several years from 1998 to 2004 and, in particular, during a spectroscopic multisite campaign in 2000. In this paper we present and analyse the data. We observed several outbursts including an intense one in 2000. Moreover, we found several periods of short-term variations, including two frequencies at 2.95 and 2.6 c d-1, which are well reproduced by models of non radial pulsations with a retrograde mode with l=3 and m=3 and a zonal mode with l=3 or 4 and m=0, respectively. The stellar rotation is probably also identified at f˜1.5 c d-1, which is coherent with the rotation frequency deduced from our determination of stellar parameters. The peak-to-peak amplitude of variations also seems to vary in time, maybe due to a beating effect between close frequencies, but the resolution in time of our data does not allow us to separate such close frequencies. Finally, a longer timescale variation may be present, with a period around 11 years, which could be associated with a binary companion.
Full text: http://www.aanda.org/articles/aa/pdf/2005/25/aa1901-04.pdf

## 2004JAVSO..33...48M - Monitoring of Mira Variable Stars

Mais, D. E.; Stencel, R. E.; Richards, D.
Abstract: We have begun intensive V- and R-band CCD monitoring of Mira variable stars since early in 2003. This project was initiated in the hopes of improving the statistics of putative flaring phenomena among these stars. This paper will give an update of the project and describe the strategies being employed.

Pollmann, E.

Pollmann, Ernst

Pollmann, Ernst

## 2004AAS...204.8502M - Mira Variable Stars: Spectroscopic and Photometric Monitoring of this broad class of Long Term Variable and Highly Evolved Stars.

Mais, D. E.; Stencel, R. E.; Richards, D.
Abstract: Mira variable stars are a broad class long period variable stars, which encompass spectroscopic classes of type M, S and C. Recently, evidence has accumulated to suggest that Mira variables may go through flare up stages which result in brightening on the order of several tenths of a magnitude or more and may last hours to days in length (Schaefer, B., 1991, Maffei, P., and Tosti, G., 1995 and de Laverny, P., et. al., 1998). Very little is known about these events, indeed it is not clear that these events are real. If they are real events, the spectroscopic changes, which occur during these flare-up episodes, remain relatively unexplored. This project was initiated in order to monitor a group of program stars of these classes in the V and R photometric bands in the hopes of "catching" some of these stars during one of these flare ups, thus offering confirmation to their reality and to be able to conduct spectral analysis of the flare-ups in real time and compare these spectra to the non-flare spectra. Monitoring of a group of these stars was carried out using equipment readily available to amateurs, both in the way of telescopes, CCD cameras and software. Commercially available software was used to control telescope pointing and image acquisition with different filters. In addition, in order to make analysis as real time as possible, scripts for reduction of images were created to automatically perform astrometric solutions and determine magnitudes of the variables from standard stars in the field. During the course of the past year, nearly 98 program stars have been monitored to address the potential flare up episodes. These include 25 M-type, 16-S type and 57 C-type Mira's. Precision of these measurements are in the milli-magnitude regime. This talk will describe the results obtained so far.

## 2004AAS...204.3504M - Amateur Spectroscopy: What is Achievable from the Backyard?

Mais, D. E.; Stencel, R. E.
Abstract: Recent advances in technology have opened the doors for amateurs to potentially contribute in the area of spectroscopy. This is due to both a shift in the use of more sensitive CCD detectors and the recent availability of powerful and versatile spectrometers aimed at the amateur community. We will focus on the instrument produced by Santa Barbara Instrument Group (SBIG), the Self-Guided Spectrometer (SGS). This instrument appeared on the market about four years ago aimed at a sub group of amateurs. In conjunction with SBIG CCD cameras, the SGS is self-guiding in that it keeps the image of an object locked onto the entrance slit, which allows for long exposures to be taken. The SGS allows spectra to be obtained with only modest aperture instruments of stars down to 10-12 magnitude. In addition, the SGS features a dual grating carousal which, with the flip of a lever, allows you to obtain dispersions in the low-resolution mode ( 4 Angstroms/pixel) or higher resolution mode ( 1 Angstrom/pixel). In the low-resolution mode, about 3000 Angstrom coverage is obtained whereas in the high-resolution mode, about 750 Angstroms. The area of the visible and near infrared part of the spectrum you decide to obtain a spectrum is dialed in by the user. More recently, swappable grating carousals have allowed for gratings with even higher dispersions (0.5 -0.3 Angstroms/pixel). The lower resolution mode is useful for stellar classification and obtaining spectra of planetary nebula. In the high-resolution modes, many absorption lines are visible of atoms, ions and simple molecules. In addition, one can measure the Doppler shift of absorption and emission lines to determine velocities of approach or recession of objects along with rotation velocities of stars and planets. Our particular interests have focused on identifying chemical elements/ions and compounds in the atmospheres of stars and nebulae. The resolution and sensitivity of the instrument is such that we have been able to identify the unstable element technetium in certain S and C type stars along with anomalous 12C/13C ratios as measured by absorption bands of diatomic carbon (C2). Measurements of certain line intensity ratios in planetary nebula allows for the calculation of both the nebula temperature and electron density. Our presentation will go into detail on the use of the SGS, its calibration and some of the kinds of measurements that can be made with an amateur sized telescope equipped with such "off the shelf" instrument.

## 2004A&A...416..669B - Properties and nature of Be stars. XXII. Long-term light and spectral variations of the new bright Be star HD 6226

Bozic, H.; Harmanec, P.; Yang, S.; Ziznovský, J.; Percy, J. R.; Ruvdjak, D.; Sudar, D.; Slechta, M.; Skoda, P.; Krpata, J.; Buil, C.
Abstract: Photometric and spectroscopic monitoring of the B star HD 6226 resulted in the finding that this object is a new bright Be star with a clear positive correlation between the brightness and emission-line strength. The emission-line episodes are relatively short and seem to repeat frequently which makes this star an ideal target for studying the causes of the Be phenomenon. The general character of the light variations, the low v sin i = 70 km s-1 and the very pronounced line asymmetries of the He I 6678 line, seen both outside and during emission-line episodes, are all attributes which make HD 6226 phenomenologically very similar to the well-known Be star omega CMa. Radial velocities of the deepest parts of the metallic and He I 6678 absorption lines vary with a strict period of 2.61507 d over the whole time interval covered by the observations, the velocities of the broad outer wings of the same lines varying in anti-phase and with a lower amplitude. This periodicity could not be found in the radial-velocity variations of the sharp core of Halpha. There is some indication of variability on a time scale of 24-29 days but our data are insufficient to prove that conclusively. A comparison of the line spectrum obtained outside emission episodes with synthetic spectra, standard dereddening of U BV magnitudes and Hipparcos parallax all agree with the conclusion that HD 6226 is a star with the following basic properties: Teff ,= 17 000 K, log g = 3.0 [cgs], mass of 5m.s and radius of 11 R&sun;. The strong emission-line episodes may appear regularly, in a cycle of 630 days but with different durations of individual cycles. HD 6226 is probably one of the first B stars for which the Be nature was predicted on the basis of the character of its light and colour changes. Based on spectral and photometric observations from the following observatories: Castanet-Tolosan, Dominion Astrophysical Observatory, Heidelberg, Hvar, Ondrejov, Skalnaté Pleso and Stará Lesná and also on photoelectric photometry by AAVSO members.
Full text: http://www.aanda.org/articles/aa/pdf/2004/11/aa3985.pdf

## 2003SASS...22...55M - Mira Variable Stars: Spectroscopic and Photometric Monitoring of this Broad Class of Long Term Variable and Highly Evolved Stars

Mais, D. E.; Stencel, R. E.; Richards, D.
Abstract: Mira variable stars are a broad class of stars, which encompass spectroscopic classes of type M, S and C. These stars are closely related in terms of their long term variability, position on the Hertzsprung-Russell diagram their intermediate mass (from ~0.8 to ~8 solar mass) and the fact that class M evolves into the S and C type stars as certain stages of shell burning around the core proceeds. These shell burning episodes produce heavy elements beyond iron and also carbon which can appear at the surface of these stars during periods of convective instability resulting in greatly enhanced abundances of elements beyond the iron group and an increase in the carbon/oxygen ratio. In addition, it is suspected that these type stars, in particular, the M type Mira's can flare up over periods of hours to days by several tenths of a mag- nitude or more. The spectroscopic changes, which occur during these flare ep- isodes, ultimately driven by core burning evolution, remain relatively un- explored. This project was initiated in order to monitor a group of program stars of these classes in the V and R photometric bands in the hopes of "catching" some of these stars during one of these flare ups and thus to be able to conduct spectral analysis of the flare-ups in real time and compare these spectra to the non-flare spectra. This talk will describe the back- ground of these type stars, in particular, their evolutionary history and their spectroscopic differences. In addition, the strategies and initiation of this project will be described.

## 2003IBVS.5398....1P - VV Cep Outside Eclipse

Pollmann, E.

Full text: http://www.konkoly.hu/cgi-bin/IBVSpdf?5398

## 2003IBVS.5374....1P - Long-term Behavior of Halpha Emission in BU Tau

Pollmann, Ernst

Full text: http://www.konkoly.hu/cgi-bin/IBVSpdf?5374

## 2003eaa..bookE5522G - Amateur Spectroscopy

Gavin, M.
Abstract: Spectroscopy (see ASTRONOMICAL SPECTROSCOPY) has seen a revival of late. Pioneers in the 19th century such as Angelo Secchi and William Huggins observed spectra visually via large refractors under pristine skies. While the eye can comprehend the brilliant solar spectrum and a few brighter stars aided by a telescope, even low spectral dispersion greatly dilutes starlight. Photo-film can marginally...
Full text: http://eaa.crcpress.com/default.asp?action=summary&articleId=5522

Pollmann, E.

Pollmann, E.

## 2003A&A...408..305M - Spectroscopy of the growing circumstellar disk in the delta Scorpii Be binary

Miroshnichenko, A. S.; Bjorkman, K. S.; Morrison, N. D.; Wisniewski, J. P.; Manset, N.; Levato, H.; Grosso, M.; Pollmann, E.; Buil, C.; Knauth, D. C.
Abstract: We present the results of a spectroscopic monitoring program of the binary system delta Scorpii, whose primary became a Be star after the last periastron encounter in the Summer of 2000. The observations cover a period of 2 years (March 2001-June 2003) and are a continuation of our previous campaign reported in Miroshnichenko et al. (\cite{metal}). We found that the emission-line spectrum was gradually strengthening over the whole monitoring period. Several short-term increases of the line emission, possibly due to outbursts of matter ejected from the stellar surface, were detected. The outbursts seem to be responsible for the brightness fadings, seen afterwards. We attempt to explain the overall observed line and continuum behaviour in terms of a circumstellar disk, growing in density and size. The disk is most likely Keplerian with an outer radius of ~10 Rstar and a mean expansion speed of ~ 0.4 km s-1.
Full text: http://www.aanda.org/articles/aa/pdf/2003/34/aa3813.pdf

## 2002SASS...21...67M - Amateur Spectroscopy: From Qualitative to Quantitative Analysis

Mais, D. E.
Abstract: Spectroscopy is a new field of study for the amateur. This type of explor- ation by an amateur is the result of the availability of several types of off-the-shelf spectrometers, which can be coupled to a CCD camera. For the most part, amateurs pursuing this area have done so more from a qualitative standpoint: stellar classification and identification of the more prominent emission and absorption lines in stars and gas clouds. However, a spectrum contains much more valuable information about the physics of the region under survey. My talk will describe my initial efforts in the use of synthetic spectroscopy and how it can be used to determine a variety of stellar para- meters such as temperature and abundances. The process involves the creation of stellar atmospheric models where a variety of variables can be altered and the resulting spectrum fitted to the actual spectrum obtained at the tele- scope to find the best fit.

## 2002IAUC.7972....4Y - V4742 Sagittarii = Possible Nova in Sagittarius

Yamaoka, H.; Monard, B.; Buil, C.; Kato, T.; Schmeer, P.; Shida, R. Y.; Pearce, A.
Abstract: C. Buil, France, reports that a spectrum obtained on Sept. 16.806 yields an expansion velocity of 1100 +/- 150 km/s from the FWHM of the H-alpha line, which shows a P-Cyg profile. T. Kato, Kyoto University, remarks that Buil's spectrum appears to be that of a nova just prior to maximum.
Full text: http://www.cbat.eps.harvard.edu/iauc/07900/07972.html#Item4

Pollmann, Ernst

## 2002BAVSR..51..116P - Koordinierte Zusammenarbeit zwischen den VdS-FG 'BAV' und 'Spektroskopie' ?

Pollmann, E.; Hanisch, R.

## 2002AsNow..16c..52M - Amateur astronomical spectroscopy

Mais, Dale E.
Abstract: Focus: spectroscopy: The author explains how the discipline spectroscopy has opened up to amateurs.

## 2002A&A...387..580H - Properties and nature of Be stars. XXI. The long-term and the orbital variations of V832 Cyg = 59 Cyg

Harmanec, P.; Bozic, H.; Percy, J. R.; Yang, S.; Ruzdjak, D.; Sudar, D.; Wolf, M.; Iliev, L.; Huang, L.; Buil, C.; Eenens, P.
Abstract: An analysis of numerous homogenized UBV photoelectric observations and red spectra of the Be star V832 Cyg from several observatories led to the following principal findings: 1. Pronounced long-term light and colour variations of V832 Cyg result from a combination of two effects: from the gradual formation of a new Be envelope, and from an asymmetry and a slow revolution of the envelope (or its one-armed oscillation). The colour variations associated with the envelope formation are characterized by a positive correlation between brightness and emission strength, typical for stars which are not seen roughly equator-on. 2. The V magnitude observations prewhitened for the long-term changes follow a sinusoidal orbital light curve with a small amplitude and a period of 28.1971d which is derived from observations spanning 43 years. This independently confirms a 12-year old suggestion that the star is a spectroscopic binary with a 29-d period. V832 Cyg thus becomes the fifth known Be star with cyclic long-term V/R variations, the duplicity of which has been proven, the four other cases being zeta Tau, V923 Aql, gamma Cas and X Per. Therefore, the hypothesis that the long-term V/R variations may arise due to the attractive force of the binary companion at certain phases of the envelope formation is still worth considering as a viable alternative to the model of one-armed oscillation. 3. We have shown that the RV and V/R variations of the Halpha and He I 6678 emission lines are all roughly in phase. In particular, the He I 6678 emission also moves with the Be primary which differs from what was found for another Be binary, \varphi Per. 4. We derived the orbital elements and found that in spite of the remaining uncertainties, the basic physical properties of the 28.2d binary are well constrained. 5. The light minimum of the orbital light curve occurs at elongation when the Be star is approaching us and the object becomes bluest in (B-V) and reddest in (U-B) at the same time. This may indicate that a part of the optically thick regions of the envelope is eclipsed at these orbital phases. Guest investigator, Dominion Astrophysical Observatory, Herzberg Institute of Astrophysics, National Research Council of Canada. Also based on observations from Castanet-Tolosan, Hvar, Ondrejov, Pic-du-Midi, Rozen, San Pedro Mártir, Toronto and Xing-Long Observatories and on photoelectric photometry by AAVSO members.
Full text: http://www.aanda.org/articles/aa/pdf/2002/20/aa2312.pdf

Pollmann, Ernst

Mais, Dale

Gavin, Maurice

Gavin, M. V.

Gavin, M. V.

Mais, D. E.

Buil, Christian

Pollmann, Ernst

Pollmann, Ernst

Gavin, Maurice

## 1999JBAA..109R.160M - Meeting contribution: Asteroidal occultations and quasar redshifts from UK amateurs

McGee, H.; Gavin, M.

## 1999JBAA..109..320G - Spectra of Wolf-Rayet stars and planetary nebulae

Gavin, M. V.
Abstract: Some spectrograms of Wolf-Rayet (WR) stars and planetary nebulae (PNe) are captured with a home-made spectroscope attached to a Schmidt-Cassegrain telescope, and the spectra are briefly analysed. The construction and potential of a low resolution stellar spectroscope is discussed together with techniques to capture images.

## 1999JBAA..109..177G - Spectra of the supernova SN1999by

Gavin, M.
Abstract: Spectra of SN1999by by Maurice Gavin. 30cm SCT+Rainbow grating+MX9 CCD; dispersion 4nm/pixel. 1999 May 2, 6, 10; 15m-35m exp. Spectrogram [at top] electronically stretched; profiles via Pixwin software.

Pollmann, E.

## 1999AsNow..13...17G - Taking the stars' fingerprints.

Gavin, M.
Abstract: The author reviews the Rainbow Optics grating. It is a transmission type of negligible thickness and can form a spectrum without special optics.

Pollmann, E.

Gavin, M.

Gavin, M.

Gavin, M. V.

Pollmann, E.

Pollmann, Ernst

Pollmann, E.

## 1996JPL96-3vol2 - The Archive of The Amateur Observation Network of The International Halley Watch, Volume 2: Comet Halley

Buchanan, T.
Abstract: February 9, 1996. National Aeronautics and Space Administration, Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California ; JPL Publication 96-3, Vol. 2; Stephen J. Edberg, Editor

Gavin, M.

Pollmann, E.

Pollmann, E.

Pollmann, E.

Gavin, M.

Pollmann, E.

Pollmann, E.

## 1994IAUS..162..282S - First results of an international multisite multitechnique campaign on omicron And

Sareyan, J. P.; Chauville, J.; Briot, D.; Adelman, S. J.; Alvarez, M.; Balega, I.; Balega, Y.; Bardin, D.; Belkin, I.; Bonneau, D.; Bossi, M.; Desnoux, V.; Espoto, M.; Fried, R.; Gonzalez-Bedolla, S.; Guo, X. Z.; Guo, Y. L.; Hao, J. X.; Huang, L.; Klotz, A.; Leister, N.; Morand, F.; Mourard, D.; Vakili, F.; Valera, F.; Zhao, F. Y.

## 1994aks..1995.....T - Spektroskopische Beobachtungen der zeta Aur-Bedeckung 1993.

Timm-Arnold, P.; Pollmann, E.

Pollmann, E.

Gavin, M.

## 1985Stern..61..108B - Praktische Leuchtkraftklassifikation für Amateurastronomen.

Böhme, D.; Pollmann, E.

Pollmann, E.

Pollmann, E.

## 1982S&W....21...83A - Spectroscopic observations regarding Mira Ceti

Alteweier, D.; Pollmann, E.; Timm, K.-P.
Abstract: Attention is given to spectroscopic studies of the variable which were conducted on October 3, 1980, and August 31, 1981, at the time of the maximum. The spectra were photoelectrically scanned with a photometric device partly constructed by the authors. Special characteristics of the recorded spectra are related to differences concerning the intensity of the TiO bands and the disappearance of the H-gamma emission line. The possible reasons for these characteristics are discussed, taking into account differences in the source surface temperature at the two times of observation. Attention is also given to the possible presence of dust or graphite particles in the stellar atmosphere. The considered investigation attempts to demonstrate that amateur astronomy does not have to be restricted to observations. Questions concerning the phenomena responsible for the observational findings should also be considered.

Gavin, M. V.

## 1978Orion..36....9P - Applied spectral classification

Pollmann, E.
Abstract: Astronomical spectroscopy is often taught only in terms of theory. This paper presents a method to teach its practical applications by using the pulsating variable, Delta-Cephei as an example. Photographic techniques are described for recording the spectral image, noting that the line spectrum of Delta-Cephei conforms to the usual classification pattern, in that the lines of a two line series grow weaker and stronger, respectively, with progressing spectral class.

## 1978Orion..36....4P - Stellar spectroscopy

Pollmann, E.
Abstract: Methods of stellar spectroscopy which are available to the amateur, i.e., are cheap and simple to operate, are outlined with reference to their accuracy. The principles of light diffraction through a prism are reviewed, and spectrographic methods based on these principles are described, including projection, and a microscope with micrometer slits. Attention is given to the photometric registration method, which can be employed with a telescope objective.

Pollmann, E.