Astronomy and Astrophysics – Astronomy
Scientific paper
May 1984
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984apj...280..825b&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 280, May 15, 1984, p. 825-847. Research supported by the Science and Engine
Astronomy and Astrophysics
Astronomy
198
Stellar Evolution, Stellar Models, Stellar Structure, Supermassive Stars, Black Holes (Astronomy), Gravitational Collapse, Helium, Mathematical Models, Point Sources, Stellar Cores, Stellar Mass Ejection
Scientific paper
The structure and evolution of Very Massive Objects (stars of 100-100,000 solar masses) are discussed in terms of simple semianalytic models. The helium enrichment due to mass loss is estimated and evidence is presented for a dynamical instability arising in the hydrogen shell burning phase of a 500 solar-mass Population I star. The fate of a VMO is decided in its oxygen core phase. Calculations of the effects of the pair instability, oxygen and silicon burning, and alpha-quenching on the global binding energy of initially isentropic polytropic cores lead to the prediction that the critical oxygen core mass above which complete collapse to a black hole occurs is about 100 solar masses corresponding to an initial star mass greater than 200 solar masses. Cores smaller than this explode; the kinetic energy liberated is estimated.
Arnett David. W.
Bond Richard J.
Carr Bernard J.
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