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Title:
Relations among stellar X-ray emission observed from Einstein, stellar rotation and bolometric luminosity
Authors:
Pallavicini, R.; Golub, L.; Rosner, R.; Vaiana, G. S.; Ayres, T.; Linsky, J. L.
Affiliation:
AA(Harvard-Smithsonian Center for Astrophysics, Cambridge, MA; Arcetri, Osservatorio Astrofisico, Florence, Italy), AB(Harvard-Smithsonian Center for Astrophysics, Cambridge, MA), AC(Harvard-Smithsonian Center for Astrophysics, Cambridge, MA), AD(Harvard-Smithsonian Center for Astrophysics, Cambridge, MA; Palermo, Osservatorio Astronomico, Palermo, Italy)
Publication:
Astrophysical Journal, Part 1, vol. 248, Aug. 15, 1981, p. 279-290. Research supported by the Consiglio Nazionale delle Richerche and Smithsonian Institution; (ApJ Homepage)
Publication Date:
08/1981
Category:
Astrophysics
Origin:
STI
NASA/STI Keywords:
Bolometers, Heao 2, Stellar Luminosity, Stellar Rotation, X Ray Astronomy, X Ray Stars, Chromosphere, Early Stars, F Stars, Hertzsprung-Russell Diagram, Late Stars, Main Sequence Stars, Stellar Coronas
Comment:
A&AA ID. AAA030.142.014
DOI:
10.1086/159152
Bibliographic Code:
1981ApJ...248..279P

Abstract

The correlation between observed stellar X-ray luminosities, bolometric luminosities, and projected rotational velocities for stars of various spectral types and luminosity classes are determined. Early type stars (O3 to A5) have X-ray luminosities independent of rotational velocities, and correlating with bolometric luminosities. Late type stars of spectral type G to M have luminosities well correlated to equatorial rotational velocities, and are independent of luminosity class. The dependence of late type stars is found to be equivalent to a relation between the X-ray surface flux and the stellar angular velocity. F stars are intermediate with X-ray luminosities higher than would be predicted on the basis of the early type star relation, although lower than expected from the late type velocity dependence. The location of RS CVn stars as a class is also discussed, and it is found that the heating of late type stellar coronas does not result from direct conversion of ratational energy.

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