X-rays from accretion of red giant winds

Details X-rays from accretion of red giant winds X-rays from accretion of red giant winds

Dec 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984apj...287..785j&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 287, Dec. 15, 1984, p. 785-792. Research supported by the Alfred P. Sloan F

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33

Binary Stars, Omicron Ceti Star, Red Giant Stars, Stellar Mass Accretion, Stellar Winds, Variable Stars, X Ray Sources, Computational Astrophysics, Eddington Approximation, Interstellar Matter, Late Stars, Main Sequence Stars, Stellar Mass Ejection, White Dwarf Stars

Scientific paper

X-ray observations of the late-type red giants Mira and R Aqr obtained with the Einstein Observatory are presented, and the general problems of white dwarf accretion from late-type giant winds is considered. The extremely low measured luminosities obtained for the two systems leads to the conclusion that the companions of Mira and R Aqr are most likely low-mass main sequence objects rather than white dwarfs as is usually assumed. The expected X-ray luminosities of true red giant/white dwarf systems are considered, and it is concluded that far too few have been detected if the canonical accretion scenario is adopted. A possible explanation of this situation in terms of grain-dominated Eddington-limited accretion is proposed.

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