Quasi-Stationary Evolution of Neutrino-Driven Supernovae

Details Quasi-Stationary Evolution of Neutrino-Driven Supernovae Quasi-Stationary Evolution of Neutrino-Driven Supernovae

Oct 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995pasj...47..581s&link_type=abstract

Publications of the Astronomical Society of Japan, v.47, p.581-588.

Astronomy and Astrophysics

Astronomy

5

Neutrinos, Shock Waves, Supernovae

Scientific paper

The flow and accretion shock above the neutrino sphere in core collapse supernovae are investigated under the assumption of spherical symmetry. By expanding physical variables (density, velocity, and internal energy) in a power series of a small parameter, the ratio of the acceleration of matter by neutrinos to the gravitational acceleration, equations are derived in such a way as to describe the thermal evolution of the shocked flow. It follows that the flow becomes almost stationary, and undergoes a quasi-stationary evolution on the time scale of the neutrino heating, as has been shown in numerical simulations. The conditions for the shock front to propagate outward are deduced from one of these equations. It is found that there exists a critical neutrino luminosity as a function of time with which the shock marginally becomes stalled. The critical luminosity is sensitive to the adiabatic index \(\gamma\) in the adiabatic preshocked flow. A smaller \(\gamma\) requires larger luminosities for a revival of the shock. It is suggested that there must be a region with \(\gamma\) very close to 4/3 (\(\ge 1.33\)) at a few hundred km from the center within a few seconds after a bounce leading to a supernova.

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