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The role of complex magnetic topologies on stellar spin-down

Published online by Cambridge University Press:  09 September 2016

Victor Réville ,
Allan Sacha Brun ,
Antoine Strugarek ,
Sean P. Matt ,
Jérôme Bouvier ,
Colin P. Folsom  and
Pascal Petit
Victor Réville
Affiliation:
Laboratoire AIM, DSM/IRFU/SAp, CEA Saclay, email: [email protected]
Allan Sacha Brun
Affiliation:
Laboratoire AIM, DSM/IRFU/SAp, CEA Saclay, email: [email protected]
Antoine Strugarek
Affiliation:
Laboratoire AIM, DSM/IRFU/SAp, CEA Saclay, email: [email protected] Département de physique, Université de Montréal
Sean P. Matt
Affiliation:
Department of Physics and Astronomy, University of Exeter
Jérôme Bouvier
Affiliation:
IPAG, Université Joseph Fourier Grenoble
Colin P. Folsom
Affiliation:
IPAG, Université Joseph Fourier Grenoble
Pascal Petit
Affiliation:
IRAP, CNRS - Université de Toulouse
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Abstract

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The rotational braking of magnetic stars through the extraction of angular momentum by stellar winds has been studied for decades, leading to several formulations. We recently demonstrated that the dependency of the braking law on the coronal magnetic field topology can be taken into account through a simple scalar parameter: the open magnetic flux. The Zeeman-Doppler Imaging technique has brought the community a reliable and precise description of the surface magnetic field of distant stars. The coronal structure can then be reconstructed using a potential field extrapolation, a technique that relies on a source surface radius beyond which all field lines are open, thus avoiding a computationally expensive MHD simulations. We developed a methodology to choose the best source surface radius in order to estimate open flux and magnetic torques. We apply this methodology to five K-type stars from 25 to 584 Myr and the Sun, and compare the resulting torque to values expected from spin evolution models.

Keywords

stars: coronaerotationmagnetic fieldslow-massmass loss
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 11 , Symposium S320: Solar and Stellar Flares and their Effects on Planets , August 2015 , pp. 297 - 302
Copyright
Copyright © International Astronomical Union 2016 

References

Arden, W. M., Norton, A. A., & Sun, X. 2014, JGR (Space Physics), 119, 1476 Google Scholar
Bouvier, J., Forestini, M., & Allain, S. 1997, A&A, 326, 1023 Google Scholar
Cohen, O. 2015, Solar Physics, arXiv:1507.00572Google Scholar
DeRosa, M. L., Brun, A. S., & Hoeksema, J. T. 2012, ApJ, 757, 96 CrossRefGoogle Scholar
Donati, J.-F. & Brown, S. F. 1997, A&A, 326, 1135 Google Scholar
Folsom, C. P., Petit, P., Bouvier, J., et al. 2016, MNRAS, 457, 580 CrossRefGoogle Scholar
Gallet, F. & Bouvier, J. 2013, A&A, 556, A36 Google Scholar
Hoeksema, J. T., Wilcox, J. M., & Scherrer, P. H. 1983, JGR, 88, 9910 CrossRefGoogle Scholar
Holzwarth, V. & Jardine, M. 2007, A&A, 463, 11 Google Scholar
Irwin, J. & Bouvier, J. 2009, in IAU Symposium, Vol. 258, 363CrossRefGoogle Scholar
Kawaler, S. D. 1988, The Astrophysical Journal, 333, 236 CrossRefGoogle Scholar
Lee, C. O., Luhmann, J. G., Hoeksema, J. T., et al. 2011, Solar Physics, 269, 367 Google Scholar
Matt, S. & Pudritz, R. E. 2008, ApJ, 678, 1109 Google Scholar
Matt, S. P., Brun, A. S., Baraffe, I., Bouvier, J., & Chabrier, G. 2015, ApJL, 799, L23 Google Scholar
Matt, S. P., Pinzón, G., Greene, T. P., & Pudritz, R. E. 2012, ApJ, 745, 101 CrossRefGoogle Scholar
Parker, E. N. 1958, ApJ, 128, 664 CrossRefGoogle Scholar
Reiners, A. & Mohanty, S. 2012, ApJ, 746, 43 CrossRefGoogle Scholar
Réville, V., Brun, A. S., Matt, S. P., Strugarek, A., & Pinto, R. F. 2015a, ApJ, 798, 116 Google Scholar
Réville, V., Brun, A. S., Strugarek, A., et al. 2015b, Accepted in ApJ, arXiv:1509.06982 Google Scholar
Riley, P., Linker, J. A., Mikić, Z., et al. 2006, ApJ, 653, 1510 Google Scholar
Sakurai, T. 1985, A&A, 152, 121 Google Scholar
Schatzman, E. 1962, Annales d'Astrophysique, 25, 18 Google Scholar
Skumanich, A. 1972, ApJ, 171, 565 Google Scholar
Titov, V. S., Mikic, Z., Török, T., Linker, J. A., & Panasenco, O. 2012, ApJ, 759, 70 CrossRefGoogle Scholar
Vidotto, A. A., Jardine, M., Morin, J., et al. 2014, MNRAS, 438, 1162 Google Scholar
Wang, Y.-M. & Sheeley, N. R. Jr. 1990, ApJ, 355, 726 Google Scholar
Weber, E. J. & Davis, L. Jr. 1967, ApJ 148 217 Google Scholar