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Imaging stellar coronae from eclipsing binary X-ray light curves

Published online by Cambridge University Press:  25 May 2016

M. Siarkowski
M. Siarkowski*
Affiliation:
Space Research Center, Polish Academy of Sciences Kopernika 11, 51-622 Wroclaw, Poland

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The Sun is the only star whose X-ray emitting, strongly inhomogenous corona can be spatially resolved via direct observations. For other late type-stars it is known that coronae do exist, but the spatial distribution of their emission is largely unknown. However in the case of eclipsing binaries this spatial structure can be potentially deduced from the orbital modulation of the observed X-ray light curve. The best candidates for this kind of analysis are RS CVn binaries, the most active and luminous late-type X-ray coronal sources. These are detached binaries with periods typically between 0.5 and 20 days, in which one or both stars have evolved into subgiant or giant of spectral type G or K. For short orbital periods (< 14 days) the tidal forces lead to synchronization of the orbital and rotational periods, so these systems rotate rigidly.

Type
Session IV: “Outer Atmospheric Structure”
Information
Symposium - International Astronomical Union , Volume 176: Stellar Surface Structure , 1996 , pp. 469 - 476
Copyright
Copyright © Kluwer 1996 

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