Types I and II supernovae and the neutrino mechanism of thermonuclear explosion of degenerate carbon-oxygen stellar cores |
| |
| Authors: | V M Chechetkin S S Gershtein V S Imshennik L N Ivanova M Yu Khlopov |
| |
| Institution: | (1) Institute for High Energy Physics, Moscow, U.S.S.R. |
| |
| Abstract: | The present work studies the hydrodynamic process of thermonuclear explosion of hydrostatic equilibrium, degenerate carbon-oxygen
cores withM
C=1.40M
⊙ with different values of central densityϱ
c
within the interval 2 × 109 <ϱ
c
< 3 × 1010 g cm−3. The initial temperature distribution has been determined by the preceding thermal stage of explosion. The calculations successively
include the kinetics of thermonuclear burning, the kinetics of β-processes, and neutrino energy losses. By considering the
neutrino mechanism of heating and carbon ignition we obtained in our numerical hydrodynamic calculations two characteristic
versions of the development of an explosion: (a) at 2 × 109 <ϱ
c
< 9 × 109 g cm−3 there is disruption of the whole star with either complete or partial burning of the carbon and a 1050–1051 erg kinetic energy; and (b) at 9 × 109 <ϱ
c
< 3 × 1010 g cm−3 the stellar core collapses into a neutron star with partial outburst of the outer envelope with a smaller kinetic energy
of 1049–1050 erg. The paper proposes and details a hypothesis (the scenario of supernovae and the formation of neutron stars) on the first
version of explosion, corresponding to SNII, and on the second, supplemented by some mechanism of slow energy release into
the envelope expelled from the newly formed neutron star, corresponding to SNI. On the basis of the proposed hypothesis a
satisfactory agreement with the observed masses and energies of the supernovae envelope, their light curves and spectra, as
well as with the data on their chemical composition has been obtained. For this agreement we must assume that type I pre-supernovae
are almost bare compact carbon-oxygen stellar cores, and that type II presupernovae are red supergiants. It is most probable
that the evolution of type I pre-supernovae occurs in close binaries while the evolution of type II pre-supernovae seems to
be very similar to the evolution of a single star. |
| |
| Keywords: | |
| 本文献已被 SpringerLink 等数据库收录！ |
|
