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Probing Be star disks: new insights from Hα spectroscopy and detailed numerical models

Published online by Cambridge University Press:  12 July 2011

Carol E. Jones ,
Christopher Tycner ,
Jessie Silaj ,
Ashly Smith  and
T. A. Aaron Sigut
Carol E. Jones
Affiliation:
Dept. of Physics and Astronomy, The University of Western Ontario London, Ontario, CanadaN6A 3K7; email: [email protected]
Christopher Tycner
Affiliation:
Dept. of Physics, Central Michigan University, Mt. Pleasant, MI 48859, USA
Jessie Silaj
Affiliation:
Dept. of Physics and Astronomy, The University of Western Ontario London, Ontario, CanadaN6A 3K7; email: [email protected]
Ashly Smith
Affiliation:
Dept. of Physics, Central Michigan University, Mt. Pleasant, MI 48859, USA
T. A. Aaron Sigut
Affiliation:
Dept. of Physics and Astronomy, The University of Western Ontario London, Ontario, CanadaN6A 3K7; email: [email protected]
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Abstract

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Hα high resolution spectroscopy combined with detailed numerical models is used to probe the physical conditions, such as density, temperature, and velocity of Be star disks. Models have been constructed for Be stars over a range in spectral types and inclination angles. We find that a variety of line shapes can be obtained by keeping the inclination fixed and changing density alone. This is due to the fact that our models account for disk temperature distributions self-consistently from the requirement of radiative equilibrium. A new analytical tool, called the variability ratio, was developed to identify emission-line stars at particular stages of variability. It is used in this work to quantify changes in the Hα equivalent widths for our observed spectra.

Keywords

stars: emission-lineBeline: profilesradiative transfercircumstellar matterstars: activity
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 6 , Symposium S272: Active OB stars: structure, evolution, mass loss, and critical limits , July 2010 , pp. 398 - 399
Copyright
Copyright © International Astronomical Union 2011

References

Jones, C. E., Tycner, C., & Smith, A. D. 2011, AJ, 141, 150CrossRefGoogle Scholar
Silaj, J., Jones, C. E., Tycner, C., Sigut, T. A. A. et al. 2010, ApJS, 187, 228CrossRefGoogle Scholar
Sigut, T. A. A. & Jones, C. E. 2007, ApJ, 668, 481CrossRefGoogle Scholar