Astronomy and Astrophysics – Astrophysics
Scientific paper
Nov 1981
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981plap.rept..291c&link_type=abstract
In ESA Plasma Astrophys. p 291-296 (SEE N82-20030 10-88)
Astronomy and Astrophysics
Astrophysics
Magnetohydrodynamic Stability, Stellar Evolution, Stellar Mass Ejection, Supernova Remnants, Supernovae, Thermonuclear Explosions, Velocity Distribution, Implosions, Light Emission, Shock Waves
Scientific paper
The physics as well as astrophysics of the supernova (SN) phenomenon are illustrated with the appropriate numbers. The explosion of a star, a supernova, occurs at the end of its evolution when the nuclear fuel in its core is almost, or completely, consumed. The star may explode due to a small residual thermonuclear detonation, type I SN, or it may collapse, type I and type II SN, leaving a neutron star remnant. The type I progenitor is thought to be an old accreting white dwarf, 1.4 interior mass, with a close companion star. A type II SN is thought to be a massive young star, 6 to 10 interior mass. The mechanism of explosion is still a challenge to model, being the most extreme conditions of matter and hydrodynamics that occur presently and excessively in the universe.
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