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New insights on Be shell stars from modelling their Hα emission profiles

Published online by Cambridge University Press:  23 January 2015

J. Silaj ,
C. E. Jones ,
T. A. A. Sigut  and
C. Tycner
J. Silaj
Affiliation:
Dept. of Physics and Astronomy, The University of Western Ontario London, ON, CanadaN6A 3K7 email: jsilaj@uwo.ca
C. E. Jones
Affiliation:
Dept. of Physics and Astronomy, The University of Western Ontario London, ON, CanadaN6A 3K7 email: jsilaj@uwo.ca
T. A. A. Sigut
Affiliation:
Dept. of Physics and Astronomy, The University of Western Ontario London, ON, CanadaN6A 3K7 email: jsilaj@uwo.ca
C. Tycner
Affiliation:
Dept. of Physics, Central Michigan University Mt. Pleasant, MI 48859, USA
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Abstract

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Be shell stars are believed to be ordinary Be stars seen edge-on, which makes them particularly desirable objects for study since the uncertainty in the inclination of the rotation axis is largely eliminated. We have recently modelled high resolution Hα spectroscopic observations for eight Be shell stars, using the non-local thermodynamical equilibrium radiative transfer code Bedisk (Sigut & Jones 2007) and the new spectral synthesis package Beray (Sigut 2011). Generally, we confirm that these systems are oriented at high inclination angles, although we find that they are not necessarily as close to edge-on as initially expected.

Keywords

stars: emission-lineBeline: profilesradiative transfercircumstellar matter
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 9 , Issue S307: New windows on massive stars: asteroseismology, interferometry, and spectropolarimetry , June 2014 , pp. 457 - 458
Copyright
Copyright © International Astronomical Union 2015 

References

Halonen, R. J. & Jones, C. E. 2013, ApJ 765, 17CrossRefGoogle Scholar
Sigut, T. A. A. 2011, in Neiner, C., Wade, G., Meynet, G., & Peters, G. (eds.), IAU Symposium, Vol. 272 of IAU Symposium, pp 426–427Google Scholar
Sigut, T. A. A. & Jones, C. E. 2007, ApJ 668, 481Google Scholar