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The evolution of magnetic fields in hot stars†

Published online by Cambridge University Press:  28 July 2017

Mary E. Oksala ,
Coralie Neiner ,
Cyril Georgy Open the ORCID record for Cyril Georgy [Opens in a new window] ,
Norbert Przybilla ,
Zsolt Keszthelyi ,
Gregg Wade ,
Stéphane Mathis ,
Aurore Blazère  and
Bram Buysschaert
Mary E. Oksala
Affiliation:
Department of Physics, California Lutheran University, 60 West Olsen Road #3700, Thousand Oaks, CA 91360, USA email: moksala@callutheran.edu LESIA, Observatoire de Paris, PSL Research University, CNRS, Sorbonne Universités, UPMC Univ. Paris 06, Univ. Paris Diderot, Sorbonne Paris Cité, 5 place Jules Janssen, 92195 Meudon, France
Coralie Neiner
Affiliation:
LESIA, Observatoire de Paris, PSL Research University, CNRS, Sorbonne Universités, UPMC Univ. Paris 06, Univ. Paris Diderot, Sorbonne Paris Cité, 5 place Jules Janssen, 92195 Meudon, France
Cyril Georgy
Affiliation:
Geneva Observatory, University of Geneva, chemin des Maillettes 51, 1290 Sauverny, Switzerland
Norbert Przybilla
Affiliation:
Institut für Astro- und Teilchenphysik, Universität Innsbruck, Technikerstr. 25/8, 6020, Innsbruck, Austria
Zsolt Keszthelyi
Affiliation:
Department of Physics, Royal Military College of Canada, PO Box 17000 Station Forces, Kingston, ON K7K 0C6, Canada Department of Physics, Engineering Physics and Astronomy, Queens University, 99 University Avenue, Kingston, ON K7L 3N6, Canada
Gregg Wade
Affiliation:
Department of Physics, Royal Military College of Canada, PO Box 17000 Station Forces, Kingston, ON K7K 0C6, Canada
Stéphane Mathis
Affiliation:
LESIA, Observatoire de Paris, PSL Research University, CNRS, Sorbonne Universités, UPMC Univ. Paris 06, Univ. Paris Diderot, Sorbonne Paris Cité, 5 place Jules Janssen, 92195 Meudon, France Laboratoire AIM Paris-Saclay, CEA/DRF - CNRS - Université Paris Diderot, IRFU/SAp Centre de Saclay, 91191 Gif-sur-Yvette, France
Aurore Blazère
Affiliation:
LESIA, Observatoire de Paris, PSL Research University, CNRS, Sorbonne Universités, UPMC Univ. Paris 06, Univ. Paris Diderot, Sorbonne Paris Cité, 5 place Jules Janssen, 92195 Meudon, France Institut d’Astrophysique et de Géophysique, Université de Liège, Quartier Agora (B5c), Allée du 6 août 19c, 4000 Sart Tilman, Liège, Belgium
Bram Buysschaert
Affiliation:
LESIA, Observatoire de Paris, PSL Research University, CNRS, Sorbonne Universités, UPMC Univ. Paris 06, Univ. Paris Diderot, Sorbonne Paris Cité, 5 place Jules Janssen, 92195 Meudon, France Instituut voor Sterrenkunde, KU Leuven, Celestijnenlaan 200D, 3001, Leuven, Belgium
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Abstract

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Over the last decade, tremendous strides have been achieved in our understanding of magnetism in main sequence hot stars. In particular, the statistical occurrence of their surface magnetism has been established (~10%) and the field origin is now understood to be fossil. However, fundamental questions remain: how do these fossil fields evolve during the post-main sequence phases, and how do they influence the evolution of hot stars from the main sequence to their ultimate demise? Filling the void of known magnetic evolved hot (OBA) stars, studying the evolution of their fossil magnetic fields along stellar evolution, and understanding the impact of these fields on the angular momentum, rotation, mass loss, and evolution of the star itself, is crucial to answering these questions, with far reaching consequences, in particular for the properties of the precursors of supernovae explosions and stellar remnants. In the framework of the BRITE spectropolarimetric survey and LIFE project, we have discovered the first few magnetic hot supergiants. Their longitudinal surface magnetic field is very weak but their configuration resembles those of main sequence hot stars. We present these first observational results and propose to interpret them at first order in the context of magnetic flux conservation as the radius of the star expands with evolution. We then also consider the possible impact of stellar structure changes along evolution.

Keywords

techniques: polarimetricstars: magnetic fieldsstars: early-typesupergiantsstars: evolution
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 12 , Symposium S329: The Lives and Death-Throes of Massive Stars , November 2016 , pp. 141 - 145
Copyright
Copyright © International Astronomical Union 2017 

Footnotes

†

Based on observations obtained at the Canada-France-Hawaii Telescope (CFHT) operated by the National Research Council of Canada, the Institut National des Sciences de l’Univers of the CNRS of France, and the University of Hawaii, and at the European Southern Observatory (ESO), Chile (program ID 094.D-0274A, 094.D-0274B, 095.D-0155A, 096.D-0072A, and 097.D-0156A).

References

Alecian, E., Wade, G. A., Catala, C., Grunhut, J. H., Landstreet, J. D., Bagnulo, S., Böhm, T., Folsom, C. P., et al., 2013, MNRAS, 429, 1001 CrossRefGoogle Scholar
Blazère, A., Neiner, C., Tkachenko, A., Bouret, J.-C., & Rivinius, T., 2015, A&A, 582, A110 Google Scholar
Donati, J.-F., Semel, M., Carter, B. D., Rees, D. E., & Collier Cameron, A., 1997, MNRAS, 291, 658 Google Scholar
Featherstone, N. A., Browning, M. K., Brun, A. S., & Toomre, J., 2009, ApJ, 705, 1000 Google Scholar
Fossati, L., Castro, N., Morel, T., Langer, N., Briquet, M., Carroll, T. A., Hubrig, S., Nieva, M. F., et al., 2015, A&A, 574, A20 Google Scholar
Fossati, L., Schneider, F. R. N., Castro, N., Langer, N., Simón-Díaz, S., Müller, A., de Koter, A., Morel, T., et al., 2016, A&A, 592, A84 Google Scholar
Georgy, C., Ekström, S., Granada, A., Meynet, G., Mowlavi, N., Eggenberger, P., & Maeder, A., 2013, A&A, 553, A24 Google Scholar
Grunhut, J. H. & Neiner, C., 2015, in Nagendra, K. N., Bagnulo, S., Centeno, R., & González, M. Jesús Martínez (eds.), IAU Symposium, Vol. 305, pp 53-60CrossRefGoogle Scholar
Grunhut, J. H., Wade, G. A., Neiner, C., Oksala, M. E., Petit, V., Alecian, E., Bohlender, D. A., Bouret, J.-C., et al., 2017, MNRAS, 465, 2432 CrossRefGoogle Scholar
Lyubimkov, L. S., Lambert, D. L., Rostopchin, S. I., Rachkovskaya, T. M., & Poklad, D. B., 2010, MNRAS, 402, 1369 Google Scholar
Maeder, A., Przybilla, N., Nieva, M.-F., Georgy, C., Meynet, G., Ekström, S., & Eggenberger, P., 2014, A&A, 565, A39 Google Scholar
Morel, T., Castro, N., Fossati, L., Hubrig, S., Langer, N., Przybilla, N., Schöller, M., Carroll, T., et al., 2015, in Meynet, G., Georgy, C., Groh, J., & Stee, P. (eds.), IAU Symposium, Vol. 307, pp 342-347Google Scholar
Neiner, C., Wade, G., Marsden, S., & Blazère, A., 2016, arXiv:1611.03285Google Scholar
Soubiran, C., Le Campion, J.-F., Brouillet, N., & Chemin, L., 2016, A&A, 591, A118 Google Scholar
Wade, G. A. and Neiner, C. and Alecian, E. and Grunhut, J. H. and Petit, V. and Batz, B. d. and Bohlender, D. A. and Cohen, D. H., et al., 2016, MNRAS, 456, 2 CrossRefGoogle Scholar
Weiss, W. W., Moffat, A. F. J., Schwarzenberg-Czerny, A., Koudelka, O. F., Grant, C. C., Zee, R. E., Kuschnig, R., Mochnacki, S., et al., 2014, in Guzik, W. J., Chaplin, G. Handler, & Pigulski, A. (eds.), IAU Symposium, Vol. 301, pp 67-68Google Scholar