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Combining seismology and spectropolarimetry of hot stars

Published online by Cambridge University Press:  23 January 2015

Coralie Neiner ,
Maryline Briquet ,
Stéphane Mathis  and
Pieter Degroote
Coralie Neiner
Affiliation:
LESIA, Observatoire de Paris, CNRS UMR 8109, UPMC, Université Paris Diderot, 5 place Jules Janssen, 92190 Meudon, France email: [email protected]
Maryline Briquet
Affiliation:
LESIA, Observatoire de Paris, CNRS UMR 8109, UPMC, Université Paris Diderot, 5 place Jules Janssen, 92190 Meudon, France email: [email protected] Institut d'Astrophysique et de Géophysique, Université de Liège, Allée du 6 Août 17, Bât B5c, 4000 Liège, Belgium
Stéphane Mathis
Affiliation:
LESIA, Observatoire de Paris, CNRS UMR 8109, UPMC, Université Paris Diderot, 5 place Jules Janssen, 92190 Meudon, France email: [email protected] Laboratoire AIM Paris-Saclay, CEA/DSM - CNRS - Université Paris Diderot, IRFU/SAp Centre de Saclay, 91191 Gif-sur-Yvette, France
Pieter Degroote
Affiliation:
LESIA, Observatoire de Paris, CNRS UMR 8109, UPMC, Université Paris Diderot, 5 place Jules Janssen, 92190 Meudon, France email: [email protected] Instituut voor Sterrenkunde, Celestijnenlaan 200D, 3001 Heverlee, Belgium
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Abstract

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Asteroseismology and spectropolarimetry have allowed us to progress significantly in our understanding of the physics of hot stars over the last decade. It is now possible to combine these two techniques to learn even more information about hot stars and constrain their models. While only a few magnetic pulsating hot stars are known as of today and have been studied with both seismology and spectropolarimetry, new opportunities - in particular Kepler2 and BRITE - are emerging and will allow us to rapidly obtain new combined results.

Keywords

stars: early-typestars: magnetic fieldsstars: oscillations (including pulsations)
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. 443 - 448
Copyright
Copyright © International Astronomical Union 2015 

References

Briquet, M., Neiner, C., Aerts, C., et al. 2012, MNRAS 427, 483Google Scholar
Briquet, M., Neiner, C., Leroy, B., & Pápics, P. I. 2013, A&A 557, L16Google Scholar
Degroote, P., Conroy, K., Hambleton, K., et al. 2013, in EAS Publications Series, Vol. 64 of EAS Publications Series, p. 277CrossRefGoogle Scholar
Donati, J.-F., Semel, M., Carter, B. D., Rees, D. E. & Collier Cameron, A. 1997, MNRAS 291, 658Google Scholar
Donati, J.-F., Wade, G. A., Babel, J., et al. 2001, MNRAS 326, 1265Google Scholar
Handler, G., Shobbrook, R. R., Uytterhoeven, K., et al. 2012, MNRAS 424, 2380Google Scholar
Henrichs, H. F., de Jong, J. A., Donati, J.-F., et al. 2000, in Smith, M. A., Henrichs, H. F., & Fabregat, J. (eds.), IAU Colloq. 175: The Be Phenomenon in Early-Type Stars, Vol. 214 of Astronomical Society of the Pacific Conference Series, p. 324Google Scholar
Henrichs, H. F., de Jong, J. A., Verdugo, E., et al. 2013, A&A 555, A46Google Scholar
Mathis, S. & Zahn, J.-P. 2005, A&A 440, 653Google Scholar
Neiner, C., Alecian, E., Briquet, M., et al. 2012, A&A 537, A148Google Scholar
Neiner, C., Alecian, E., & Mathis, S. 2011, in Alecian, G., Belkacem, K., Samadi, R., & Valls-Gabaud, D. (eds.), SF2A-2011: Proceedings of the Annual meeting of the French Society of Astronomy and Astrophysics, p. 509Google Scholar
Neiner, C., Degroote, P., Coste, B., Briquet, M., & Mathis, S. 2013, in Magnetic fields throughout stellar evolution, Vol. 302 of IAU Symposium, ArXiv 1311.2262Google Scholar
Neiner, C., Henrichs, H. F., Floquet, M., et al. 2003, A&A 411, 565Google Scholar
Pápics, P. I., Briquet, M., Baglin, A., et al. 2012, A&A 542, A55Google Scholar
Savonije, G. J. 2013, A&A 559, A25Google Scholar
Shibahashi, H. & Aerts, C. 2000, ApJ (Letters) 531, L143Google Scholar
Spruit, H. C. 1999, A&A 349, 189Google Scholar
Wade, G. A., Grunhut, J., Alecian, E., et al. 2013, in Magnetic fields throughout stellar evolution, Vol. 302 of IAU Symposium, p 265Google Scholar
Weiss, W. W., Rucinski, S. M., Moffat, A. F. J., et al. 2014, PASP 126, 573Google Scholar
Zahn, J.-P. 2011, in Neiner, C., Wade, G., Meynet, G., & Peters, G. (eds.), IAU Symposium, Vol. 272 of IAU Symposium, p. 14Google Scholar