Collapsing Stellar Cores and Supernovae
- Creators
- Epstein, R. I.
- Nørgaard, H.
- Bond, J. R.
Abstract
The evolution of a stellar core is studied during its final quasi-hydrostatic contraction. The core structure and the (poorly known) properties of neutron rich matter are parametrized to include most plausible cases. It is found that the density-temperature trajectory of the material in the central part of the core (the core-center) is insensitive to nearly all reasonable parameter variations. The central density at the onset of the dynamic phase of the collapse (when the core-center begins to fall away from the rest of the star) and the fraction of the emitted neutrinos which are trapped in the collapsing core-center depend quite sensitively on the properties of neutron rich matter. We estimate that the amount of energy E_(cm); which is imparted to the core-mantle by the neutrinos which escape from the imploded core-center can span a large range of values. For plausible choices of nuclear and model parameters E_(cm) can be large enough to yield a supernova event.
Additional Information
© 1979 European Southern Observatory. Provided by the NASA Astrophysics Data System. Received April 21, 1978. We gladly acknowledge the stimulating and useful discussions we have had with Gordon Baym; Ted Mazurek, Dave Arnett, Demos Kazanas and Ken Van Riper. This work was supported in part by NSF Grants PHY 76-83685 and AST 76-21707. HN also gratefully acknowledges the support of the Danish Natural Science Research Council.Attached Files
Published - 1979A+A____74__353E.pdf
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Additional details
- Eprint ID
- 39383
- Resolver ID
- CaltechAUTHORS:20130716-082240964
- PHY 76-83685
- NSF
- AST 76-21707
- NSF
- Danish Natural Science Research Council
- Created
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2013-07-16Created from EPrint's datestamp field
- Updated
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2020-10-30Created from EPrint's last_modified field