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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 

References

Chambliss, C.R., 1976, PASP 88, 762 Google Scholar
Bedford, D.K., Jeffries, R.D., Geyer, E.H., Vilhu, O., 1990, MNRAS 243, 557 Google Scholar
Culhane, J.L., White, N.E., Shafer, R.A., Parmar, A.N., 1990, MNRAS 243, 424 Google Scholar
Guinan, E.F., Carroll, S.M., 1990, in Active Close Binaries , ed. İbanoğlu, C., Kluwer, Dordrecht, p. 7 Google Scholar
Lemen, J.R., Mewe, R., Schrijver, C.J., Fludra, A., 1989, ApJ 341, 474 Google Scholar
Ottmann, R., Schmitt, J.H.M.M., Kürster, M., 1993, ApJ 413, 710 Google Scholar
Ottmann, R., Schmitt, J.H.M.M., 1994, A&A 283, 871 Google Scholar
Pres, P., Siarkowski, M., Sylwester, J., 1995a, MNRAS 275, 43 Google Scholar
Pres, P., Siarkowski, M., Sylwester, J., 1995b, JOSO Annual Report 1994 , ed. Saniga, M., p.199 Google Scholar
Schmitt, J.H.M.M., 1992, in Variabilities in Stars and Galaxies , ed. Klare, G., Springer-Verlag, p. 188 Google Scholar
Siarkowski, M., 1992, MNRAS 259, 453 Google Scholar
Siarkowski, M., Sylwester, J., Pres, P., 1994, in Solar Coronal Structure , Proc. IAU Colloq. 144, eds. Rusin, V., Heinzel, P. and Vial, J.-C., VEDA, Bratislava, p. 207 Google Scholar
Siarkowski, M., Pres, P., White, N.E., Singh, K.P., Drake, S.A., 1995, ApJ, submitted Google Scholar
Singh, K.P., White, N.E., Drake, S.A., 1995, ApJ, submitted Google Scholar
Swank, J.H., White, N.E., Holt, S.S., Becker, R.H., 1981, ApJ 246, 214 Google Scholar
Vesecky, J.F., Antiochos, S.K., Underwood, J.H., 1979, ApJ 233, 987 Google Scholar
Walter, F.M., Gibson, D.M., Basri, G.S., 1983, ApJ 267, 665 Google Scholar
White, N.E., Shafer, R.A., Horne, K., Parmar, A.N., Culhane, J.L., 1990, ApJ 350, 776 Google Scholar
White, N.E. et al. 1994, PASJ 46, L97 Google Scholar