Discovery of X-ray emission lines from the RS CVn binary sigma CrB

Details Discovery of X-ray emission lines from the RS CVn binary sigma CrB Discovery of X-ray emission lines from the RS CVn binary sigma CrB

Sep 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981mnras.196p..73a&link_type=abstract

Monthly Notices of the Royal Astronomical Society, vol. 196, Sept. 1981, p. 73P-79P.

Astronomy and Astrophysics

Astronomy

17

Binary Stars, Emission Spectra, Line Spectra, Stellar Spectra, X Ray Sources, X Ray Spectra, Abundance, Coronal Loops, Energy Spectra, Heao 2, High Temperature Plasmas, Plasma Radiation, Spaceborne Astronomy, Stellar Coronas, Stellar Models, Stellar Temperature, Variable Stars

Scientific paper

X-ray observations of the RS CVn binary sigma CrB were carried out with a solid state spectrometer on board the Einstein Observatory in 1979. X-ray emission lines due to Mg XI, Si XIII, S XV and a blend of L-transition lines due to Fe XVII and Fe XVIII were detected in the sigma CrB spectrum. The observed X-ray spectrum is described by a two-temperature coronal X-ray emission model: the dominant low temperature component originates in a plasma at a temperature of 5.9 + or 0.5 x 10 to the 6th K; the weaker higher temperature arises from a plasma of not less than 35 x 10 to the 6th K. Intensity variations over a period of a few hours are also recorded and thought to be due to a variation in the number of loops concentrated around active regions on the star surface. Implications of the results are discussed in terms of the constant-pressure coronal loop model (Rosner, Tucker, Vaiana, 1978).

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