Type IA supernovae - Constraints on baryonic dark matter

Details Type IA supernovae - Constraints on baryonic dark matter Type IA supernovae - Constraints on baryonic dark matter

May 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991apj...372..448s&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 372, May 10, 1991, p. 448-454.

Statistics

Computation

38

Baryons, Binary Stars, Cosmology, Dark Matter, Supernovae, White Dwarf Stars, Chemical Evolution, Computational Astrophysics, Galactic Structure, Halos, Stellar Evolution, Stellar Models

Scientific paper

Models in which the dark matter of galaxy halos is in the form of white dwarfs (WDs) are examined. Major constraints, which have been previously neglected, result from the occurrence of Type Ia supernovae, which are the products of merging WDs in binary systems whose orbits decay due to the emission of gravitational wave radiation. The lack of observed supernovae in the outer regions of galaxies, together with the relatively low abundance of iron in the hot, X-ray gas of galactic halos, limit the fraction of binaries to far less than 1 percent in extant models of WD-dominated halos, for standard Type Ia parameters. This binary fraction is much smaller than that believed typical for luminous stars, necessitating a further peculiarity in the star-formation process during the formation of the dark halo.

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