The Evolution and fate of Very Massive Objects

Bond, J.R.; Arnett, W.D.; Carr, Bernard J.

doi:10.1086/162057

The Evolution and fate of Very Massive Objects

J.R. Bond
(
- Stanford U., Phys. Dept. and
- Cambridge U. and
- Chicago U.
)
,
W.D. Arnett
(
- Stanford U., Phys. Dept. and
- Cambridge U. and
- Chicago U.
)
,
Bernard J. Carr
(
- Stanford U., Phys. Dept. and
- Cambridge U. and
- Chicago U.
)

May, 1984

23 pages

Published in:

Astrophys.J. 280 (1984) 825-847

DOI:

10.1086/162057

View in:

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Abstract: (ADS)

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.

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