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Magnetic activity of interacting binaries

Published online by Cambridge University Press:  12 September 2017

Colin A. Hill
Colin A. Hill*
Affiliation:
Université de Toulouse / CNRS-INSU, IRAP / UMR 5277, F-31400, Toulouse, France email: [email protected]
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Abstract

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Interacting binaries provide unique parameter regimes, both rapid rotation and tidal distortion, in which to test stellar dynamo theories and study the resulting magnetic activity. Close binaries such as cataclysmic variables (CVs) have been found to differentially rotate, and so can provide testbeds for tidal dissipation efficiency in stellar convective envelopes, with implications for both CV and planet-star evolution. Furthermore, CVs show evidence of preferential emergence of magnetic flux tubes towards the companion star, as well as large, long-lived prominences that form preferentially within the binary geometry. Moreover, RS CVn binaries also show clear magnetic interactions between the two components in the form of coronal X-ray emission. Here, we review several examples of magnetic interactions in different types of close binaries.

Keywords

stars: novaecataclysmic variablesstars: activitystars: spotsstars: imagingstars: magnetic fieldsstars: binaries (including multiple): closetechniques: spectroscopic
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 12 , Symposium S328: Living Around Active Stars , October 2016 , pp. 54 - 60
Copyright
Copyright © International Astronomical Union 2017 

References

Brothwell, R. D., et al., 2014, MNRAS, 440, 3392 CrossRefGoogle Scholar
Hill, C. A., et al., 2016, MNRAS, 459, 1858 CrossRefGoogle Scholar
Işık, E., & and Schmitt, D. and Schüssler, M., 2011, A&A, 528, 135 Google Scholar
Saar, S. H. and Brandenburg, A., 1999, ApJ, 524, 295 CrossRefGoogle Scholar
Scharlemann, E. T, 1982, ApJ, 253, 298 CrossRefGoogle Scholar
Siarkowski, M., 1992, MNRAS, 259, 453 CrossRefGoogle Scholar
Siarkowski, M., et al., 1996, ApJ, 473, 470 CrossRefGoogle Scholar
Steeghs, D. T. H., et al., 1996, MNRAS, 281, 626 CrossRefGoogle Scholar
Watson, C. A., et al., 2007, MNRAS, 382, 1105 CrossRefGoogle Scholar