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Asymmetrical Ejection of Matter in a Thermonuclear Model of a Supernova Explosion

Published online by Cambridge University Press:  12 April 2016

V.M. Chechetkin ,
A.A. Denisov ,
A.V. Koldoba ,
Yu.A. Poveschenko  and
Yu.P. Popov
V.M. Chechetkin
Affiliation:
Institute of Applied Mathematics, USSR Academy of Sciences, Moscow, 117259
A.A. Denisov
Affiliation:
Institute of Applied Mathematics, USSR Academy of Sciences, Moscow, 117259
A.V. Koldoba
Affiliation:
Institute of Applied Mathematics, USSR Academy of Sciences, Moscow, 117259
Yu.A. Poveschenko
Affiliation:
Institute of Applied Mathematics, USSR Academy of Sciences, Moscow, 117259
Yu.P. Popov
Affiliation:
Institute of Applied Mathematics, USSR Academy of Sciences, Moscow, 117259

Extract

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With the recent Supernova 1987a in the LMC, new and interesting possibilities have arisen for the solution of a problem relating to the explosion mechanism of supernovae. The presupernova was probably a B3Ia, the blue supergiant, and not a red giant as it was earlier thought likely. Calculations of the evolution, which have been made recently, show that the loss of hydrodynamical stability may be connected with carbon burning in the stellar core during the blue giant stage. This loss of stability of the CO core is the main factor in our explanation of the recent event of SN 1987a.

Before we consider the thermonuclear model of a supernova based on a thermal flash in the degenerate CO core, let us dwell on the present situation in the theory of supernovae. The main problem in supernova theory is the simultaneity of births of a compact remnant and an expelled envelope. The compact remnant later becomes a neutron star. The expelled envelope determines the curve of brightness. Now, it is clear that a supernova explosion may result in either the total disruption of a star or in the simultaneous production of a compact remnant and an expelled envelope.

Type
Research Article
Information
International Astronomical Union Colloquium , Volume 101: Supernova Remnants and the Interstellar Medium , 1988 , pp. 27 - 30
Copyright
Copyright © Cambridge University Press 1988

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