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A Re-Analysis of the X-ray Spectrum of HR 1099 and Its Implications for Coronal Abundances

Published online by Cambridge University Press:  12 April 2016

Stephen A. Drake ,
Kulinder P. Singh  and
Nicholas E. White
Stephen A. Drake
Affiliation:
EASARC, Code 668, NASA/GSFC, Greenbelt, MD 20771, USA USRA, Code 610.3, NASA/GSFC, Greenbelt, MD 20771, USA
Kulinder P. Singh
Affiliation:
EASARC, Code 668, NASA/GSFC, Greenbelt, MD 20771, USA TIFR, Homi Bhabha Road, Colaba, Bombay, 400 005, India
Nicholas E. White
Affiliation:
EASARC, Code 668, NASA/GSFC, Greenbelt, MD 20771, USA

Abstract

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We have analyzed archival X-ray spectra of the RS CVn binary system HR 1099 in an attempt to see if we can obtain a consistent picture of the state of the X-ray emitting plasma. We have modeled six spectra obtained by the Exosat ME and LE telescopes, two spectra obtained by the Einstein SSS and MPC instruments, as well as a more recent ROSAT PSPC spectrum. We find that these spectra are in general poorly fitted by solar-abundance Raymond and Smith or Mewe and Kaastra thermal plasma models, and that no simple combination of these models significantly improves these fits: the observed continuum is too strong relative to the line features. We find acceptable fits for thermal models with two or more components in which the heavy elements are depleted by a factor of 2 to 4 relative to their solar photospheric values. These results are consistent with those obtained from the analysis of higher-resolution EUVE and ASCA spectra of active binary and single stars. We discuss the implications of these findings on ongoing analyses of the EUV spectra of HR 1099 and other RS CVn binaries.

Type
III. Coronae of Cool Stars
Information
International Astronomical Union Colloquium , Volume 152: Astrophysics in the Extreme Ultraviolet , 1996 , pp. 147 - 151
Copyright
Copyright © Kluwer 1996

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