The Early Phases of the Evolution of Hot Helium Cores

Details The Early Phases of the Evolution of Hot Helium Cores The Early Phases of the Evolution of Hot Helium Cores

Oct 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000aas...196.6309n&link_type=abstract

American Astronomical Society, 196th AAS Meeting, #63.09; Bulletin of the American Astronomical Society, Vol. 32, p.1286

Physics

Scientific paper

We examine the evolution of close binary systems containing a mass accreting compact object and a post-main-sequence donor. Using the best available input physics, we have calculated the evolutionary tracks of these systems for a wide range of metallicities and evolutionary states of the donor star (i.e., when it first starts to lose mass to its compact companion). Assuming that a sufficiently massive helium core has formed within the donor at the onset of mass transfer, the donor will be stripped of its hydrogen-rich envelope and will rapidly evolve from a cool "giant" to a relatively hot, compact object composed almost entirely of helium. Mass transfer ceases and these objects are destined to cool forever to become fully electron-degenerate helium dwarfs. A number of helium dwarfs have recently been discovered in isolation and in binary systems. We have established the range of initial conditions of the progenitors of these helium dwarfs for a wide array of core masses and metallicities. While this range of variations (for a fixed mass and metallicity) becomes unimportant to the observable properties of old helium dwarfs that have had a long time to cool, it is quite significant for young dwarfs that are quite luminous and are likely to be preferentially selected in any observational survey. This work was supported in part by the Natural Sciences and Engineering Research Council (NSERC) of Canada.

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