Abstract
A ‘Very Massive Object’, henceforth referred to as a VMO, is defined to be a star that goes pair unstable during its oxygen burning phase. This means that it must have an initial mass in the range 102–105 MƟ. The evolution of such a star, in both its hydrogen and helium burning phase (when it is subject to rapid mass loss) and its unstable oxygen burning phase has been summarized in an accompanying talk (Bond, Arnett and Carr 1982). The important qualitative conclusion is that oxygen cores with mass larger than about 102 MƟ collapse entirely to black holes, whereas oxygen cores smaller than this disrupt. The critical dividing mass MƟ associated with the precursor hydrogen star would lie in the range 200–500 MƟ, the large uncertainty reflecting our ignorance of how much mass loss occurs during the hydrogen and helium burning phase.
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Carr, B.J., Arnett, W.D., Bond, J.R. (1982). Pregalactic Very Massive Objects and Their Cosmological Consequences. In: Rees, M.J., Stoneham, R.J. (eds) Supernovae: A Survey of Current Research. NATO Advanced Study Institutes Series, vol 90. Springer, Dordrecht. https://doi.org/10.1007/978-94-009-7876-8_18
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