A post-core-collapse model for the nucleus of M33

Details A post-core-collapse model for the nucleus of M33 A post-core-collapse model for the nucleus of M33

Dec 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991natur.354..376h&link_type=abstract

Nature (ISSN 0028-0836), vol. 354, Dec. 5, 1991, p. 376, 377. Research supported by Alfred P. Sloan Foundation, NASA, NSF, and U

Computer Science

17

Cataclysmic Variables, Emission Spectra, Globular Clusters, Gravitational Collapse, X Ray Binaries, Binary Stars, Novae, Spiral Galaxies, Stellar Color, Stellar Models

Scientific paper

A model for the post-collapse core of M33 is proposed. By analogy with globular clusters, the formation of tight binary systems powers the reexpansion of the core, and it is expected that low-mass X-ray binaries form at a rate about equal to that of all galactic globular clusters combined. About a dozen such binaries should be present, and their combined emission may explain the large and enigmatic unresolved X-ray emission from the nucleus of M33. In addition, tidal formation of cataclysmic binaries may lead to a nova rate of more than about one per century. Numerous blue stragglers have probably formed through mergers caused by stellar collisions, but their density is probably too low to explain the blue color of the nucleus. Young stars are the likely cause for the color, and their presence may complicate the simple dynamical picture presented here.

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