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[en] Presupernova evolution and the hydrodynamic behavior of supernova explosions in stars having electron-degenerate cores are summarized. Carbon deflagration supernovae in C+O cores disrupt the star completely. On the other hand, in electron capture supernovae, O+Ne+Mg cores collapse to form neutron stars despite the competing oxygen deflagration. Also discussed are white dwarf models for Type I supernovae (SN I). Supernova explosions in accreting white dwarfs are either the detonation or deflagration type depending mainly on the accretion rate. The carbon deflagration model reproduces many of the observed features of SN I. (Auth.)
Source
Sugimoto, D. (Tokyo Univ. (Japan)); Lamb, D.Q. (Harvard Univ., Cambridge, MA (USA). Center for Astrophysics); Schramm, D.N. (Chicago Univ., IL (USA)) (eds.); International Astronomical Union; 362 p; ISBN 90-277-1274-3; 
; 1981; p. 295-315; D. Reidel; Dordrecht, Netherlands; International Astronomical Union symposium no. 93 on fundamental problems in the theory of stellar evolution; Kyoto, Japan; 22 - 25 Jul 1980; 69 refs.
; 1981; p. 295-315; D. Reidel; Dordrecht, Netherlands; International Astronomical Union symposium no. 93 on fundamental problems in the theory of stellar evolution; Kyoto, Japan; 22 - 25 Jul 1980; 69 refs.