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Einstein X-ray survey of the Pleiades - The dependence of X-ray emission on stellar age
Micela, G.; Sciortino, S.; Serio, S.; Vaiana, G. S.; Bookbinder, J.; Golub, L.; Harnden, F. R., Jr.; Rosner, R.
AA(Osservatorio Astronomico, Palermo, Italy), AB(Osservatorio Astronomico, Palermo, Italy), AC(Osservatorio Astronomico, Palermo, Italy; Harvard-Smithsonian Center for Astrophysics, Cambridge, MA), AD(Osservatorio Astronomico, Palermo, Italy; Harvard-Smithsonian Center for Astrophysics, Cambridge, MA), AE(Harvard-Smithsonian Center for Astrophysics, Cambridge, MA), AF(Harvard-Smithsonian Center for Astrophysics, Cambridge, MA), AG(Harvard-Smithsonian Center for Astrophysics, Cambridge, MA), AH(Harvard-Smithsonian Center for Astrophysics, Cambridge, MA)
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 292, May 1, 1985, p. 172-180. Research supported by the Consiglio Nazionale delle Ricerche and Ministero della Pubblica Istruzione. (ApJ Homepage)
Publication Date:
NASA/STI Keywords:
Pleiades Cluster, Spaceborne Astronomy, Star Clusters, X Ray Sources, Astronomical Catalogs, Dwarf Stars, G Stars, Heao 2, K Stars, Stellar Luminosity, Stellar Rotation
Bibliographic Code:


The data obtained with two pointed observations of 1 deg by 1 deg fields of the Pleiades region have been analyzed, and the results are presented. The maximum-likelihood X-ray luminosity functions for the Pleiades G and K stars in the cluster are derived, and it is shown that, for the G stars, the Pleiades X-ray luminosity function is significantly brighter than the corresponding function for Hyades G dwarf stars. This finding indicates a dependence of X-ray luminosity on stellar age, which is confirmed by comparison of the same data with median X-ray luminosities of pre-main sequence and local disk population dwarf G stars. It is suggested that the significantly larger number of bright X-ray sources associated with G stars than with K stars, the lack of detection of M stars, and the relatively rapid rotation of the Pleiades K stars can be explained in terms of the onset of internal differential rotation near the convective envelope-radidative core interface after the spin-up phase during evolution to the main sequence.

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