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Why do hot subdwarf stars pulsate?

Published online by Cambridge University Press:  27 October 2016

Stephan Geier
Stephan Geier*
Affiliation:
European Southern Observatory, Karl-Schwarzschild-Str. 2, 85748 Garching, Germany email: [email protected] Dr. Karl Remeis-Observatory & ECAP, Astronomical Institute, Friedrich-Alexander University Erlangen-Nuremberg, Sternwartstr. 7, D 96049 Bamberg, Germany
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Abstract

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Hot subdwarf B stars (sdBs) are the stripped cores of red giants located at the bluest extension of the horizontal branch. Several different kinds of pulsators are found among those stars. The mechanism that drives those pulsations is well known and the theoretically predicted instability regions for both the short-period p-mode and the long-period g-mode pulsators match the observed distributions fairly well. However, it remains unclear why only a fraction of the sdB stars pulsate, while stars with otherwise very similar parameters do not show pulsations. From an observers perspective I review possible candidates for the missing parameter that makes sdB stars pulsate or not.

Keywords

stars: subdwarfsstars: pulsators
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 11 , General Assembly A29B: Astronomy in Focus , August 2015 , pp. 521 - 524
Copyright
Copyright © International Astronomical Union 2016 

References

Blanchette, J.-P., et al. 2008, A&A, 483, 21 Google Scholar
Fontaine, G., et al. 2014, ASP Conf. Ser., 481, 19 Google Scholar
Foster, H. M., Reed, M. D., Telting, J. H., Østensen, R. H., & Baran, A. S. 2015, ApJ, 805, 94 Google Scholar
Geier, S. 2013, A&A, 549, 110 Google Scholar
Geier, S. 2015, AN, 336, 437 Google Scholar
Geier, S., et al. 2010, A&A, 519, 25 Google Scholar
Geier, S. & Heber, U. 2012, A&A, 543, 149 Google Scholar
Geier, S., et al. 2013, A&A, 554, 54 Google Scholar
Heber, U., Reid, I. N., & Werner, K. 2000, A&A, 363, 198 Google Scholar
Hu, H., Tout, C. A., Glebbeek, E., & Dupret, M.-A. 2011, MNRAS, 418, 195 Google Scholar
Mereghetti, S., et al. 2014, MNRAS, 441, 2684 Google Scholar
Pablo, H., Kawaler, S. D., & Green, E. M. 2011, ApJ, 740, L47 CrossRefGoogle Scholar
Pablo, H., et al. 2012, MNRAS, 422, 1343 Google Scholar
Østensen, R. H., et al. 2014, A&A, 569, 15 Google Scholar
Randall, S. K., Fontaine, G., Charpinet, S., van Grootel, V., & Brassard, P. 2014, IAUS, 301, 289 Google Scholar
Schaffenroth, V., et al. 2014, A&A, 570, 70 Google Scholar
Telting, J. H., et al. 2012, A&A, 544, 1 Google Scholar
Telting, J. H., et al. 2014, A&A, 570, 129 Google Scholar
Unglaub, K. & Bues, I. 2001, A&A, 374, 570 Google Scholar
Vink, J. S. & Cassisi, S. 2002, A&A, 392, 553 Google Scholar