Computer simulations of stellar collapse and supernovae explosions - Non-rotating and rotating models

Details Computer simulations of stellar collapse and supernovae explosions - Non-rotating and rotating models Computer simulations of stellar collapse and supernovae explosions - Non-rotating and rotating models

Nov 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982sscr.conf..123h&link_type=abstract

In: Supernovae: A survey of current research; Proceedings of the Advanced Study Institute, Cambridge, England, June 29-July 10,

Statistics

Computation

27

Computerized Simulation, Gravitational Collapse, Stellar Mass Ejection, Stellar Models, Stellar Rotation, Supernovae, Adiabatic Conditions, Electron Density (Concentration), Entropy, Flow Velocity, Nonadiabatic Conditions, Shock Wave Propagation, Stellar Evolution, Stellar Mass

Scientific paper

Computer simulation models of type II supernova explosions are reviewed. For nonrotating models, it is discussed whether or not a shock wave generated from the rebounding core by itself causes mass ejection. Both adiabatic and nonadiabatic models are discussed in detail. In the former, entropy is strictly conserved and weak interaction reactions are ignored. Consequently, the electron concentration stays high and a very energetic supernova explosion results. In the nonadiabatic model, most of the shock energy is consumed in dissociating heavy nuclei on the way out, the rest being radiated away by neutrinos. In none of the recent computations does a supernova explosion result; possibilities to overcome these difficulties are discussed. Then, computation in which the assumption of spherical symmetry is omitted are addressed. Rotating models are considered, and it is shown that even initially moderately rotating stellar cores add important modifications to the simple core-bounce picture. Finally, processes resulting from the presence of magnetic fields, lepton number, entropy gradients, and unburned nuclear fuel are treated.

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