Solid white dwarfs as Type I supernova progenitors

Details Solid white dwarfs as Type I supernova progenitors Solid white dwarfs as Type I supernova progenitors

May 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984natur.309..431i&link_type=abstract

Nature (ISSN 0028-0836), vol. 309, May 31, 1984, p. 431, 432. Research supported by the Ministerio de Education y Ciencia Espano

Physics

18

Binary Stars, Supernovae, White Dwarf Stars, X Ray Sources, Carbon Stars, Gravitational Collapse, Stellar Mass Accretion

Scientific paper

Mass-accreting white dwarfs in close binary systems are generally thought to be Type I supernova (SN I) progenitors. Low-mass (less than or approximately equal to 5 solar masses) binary X-ray sources (also known as Type II sources) equally appear to be the descendants of cataclysmic variables and thus to have been produced by the collapse of a mass-accreting white dwarf. It is pointed out here that a single process, thermonuclear ignition inside a partially solid, carbon-oxygen white dwarf, may account for the full range of phenomena: from mildly or non-explosive collapses leaving a condensed remnant up to 'slow' to 'fast' SN I outbursts with total disruption of the parent star.

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