Misc,
The Deaths of Very Massive Stars
(Jun 21, 2014)
Abstract
The theory underlying the evolution and death of stars heavier than 10 Msun
on the main sequence is reviewed with an emphasis upon stars much heavier than
30 Msun. These are stars that, in the absence of substantial mass loss, are
expected to either produce black holes when they die, or, for helium cores
heavier than about 35 Msun, encounter the pair instability. A wide variety of
outcomes is possible depending upon the initial composition of the star, its
rotation rate, and the physics used to model its evolution. These heavier stars
can produce some of the brightest supernovae in the universe, but also some of
the faintest. They can make gamma-ray bursts or collapse without a whimper.
Their nucleosynthesis can range from just CNO to a broad range of elements up
to the iron group. Though rare nowadays, they probably played a
disproportionate role in shaping the evolution of the universe following the
formation of its first stars.
