The collapse of white dwarfs to neutron stars

Details The collapse of white dwarfs to neutron stars The collapse of white dwarfs to neutron stars

May 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992apj...391..228w&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 391, no. 1, May 20, 1992, p. 228-235. Research supported by University of C

Astronomy and Astrophysics

Astrophysics

129

Gamma Ray Bursts, Neutron Stars, Nuclear Astrophysics, Stellar Evolution, White Dwarf Stars, Emission Spectra, Gamma Ray Spectra, Neutrinos, Stellar Luminosity, Stellar Models, Stellar Winds

Scientific paper

The observable consequences of an accreting white dwarf collapsing directly to a neutron star are considered. The outcome depends critically upon the nature of the wind that is driven by neutrino absorption in the surface layers as the dwarf collapses. Unlike previous calculations which either ignored mass loss or employed inadequate zoning to resolve it, a characteristic mass-loss rate of about 0.005 solar mass/s and an energy input of 5 x 10 exp 50 ergs/s is found. Such a large mass-loss rate almost completely obscures any prompt electromagnetic display and certainly rules out the production by this model of gamma-ray bursts situated at cosmological distances. The occurrence of such collapses with the Milky Way Galaxy might, however, be detected and limited by their nucleosynthesis and gamma-ray line emission. To avoid the overproduction of rare neutron-rich isotopes heavier than iron, such events must be very infrequent, probably happening no more than once every thousand years.

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