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An Einstein Observatory X-ray survey of main-sequence stars with shallow convection zones
Schmitt, J. H. M. M.; Golub, L.; Harnden, F. R., Jr.; Maxson, C. W.; Rosner, R.; Vaiana, G. S.
AA(Harvard-Smithsonian Center for Astrophysics, Cambridge, MA), AB(Harvard-Smithsonian Center for Astrophysics, Cambridge, MA), AC(Harvard-Smithsonian Center for Astrophysics, Cambridge, MA), AD(Harvard-Smithsonian Center for Astrophysics, Cambridge, MA), AE(Harvard-Smithsonian Center for Astrophysics, Cambridge, MA), AF(Harvard-Smithsonian Center for Astrophysics, Cambridge, MA; Osservatorio Astronomico, Palermo, Italy)
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 290, March 1, 1985, p. 307-320. (ApJ Homepage)
Publication Date:
NASA/STI Keywords:
Binary Stars, Heao 2, Main Sequence Stars, Stellar Luminosity, Stellar Rotation, X Ray Astronomy, A Stars, B Stars, Convection, F Stars, Late Stars, O Stars, X Ray Sources
Bibliographic Code:


The results of an X-ray survey of bright late A and early F stars on the main B-V sequence between 0.1 and 0.5 are presented. All the stars were observed with the Einstein Observatory for a period of at least 500 seconds. The survey results show significantly larger X-ray luminosities for the sample binaries than for the single stars. It is suggested that the difference is due to the presence of multiple X-ray sources in binaries. It is shown that the X-ray luminosities for single stars increase rapidly with increasing color, and that the relation Lx/Lbol is equal to about 10 to the -7th does not hold for A stars. No correlation was found between X-ray luminosity and projected equatorial rotation velocity. It is argued on the basis of the observations that X-ray emission in the sample stars originated from coronae. The available observational evidence supporting this view is discussed.

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