Other
Scientific paper
May 1996
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996aps..may..i104w&link_type=abstract
American Physical Society, APS/AAPT Joint Meeting, May 2-5, 1996, abstract #I1.04
Other
Scientific paper
While the idea that the chemical elements find their origin in the stars stretches back to the early part of the century, it was Fowler and Hoyle who emphasized the role of massive stars, designated and explored the two types of theoretical models for supernovae still employed (degenerate thermonuclear explosion and iron core collapse for Type I and II, respectively), and began the quantitative calculation of stellar nucleosynthesis. These calculations required a large amount of nuclear cross section information gathered, and, in many instances, measured by Willy Fowler and his colleagues. I shall briefly review our current understanding of the evolution and explosion of stars greater than 10 solar masses, emphasizing recent developments and uncertainties. The nucleosynthesis from these model stars gives overall good agreement with abundances measured in our sun and other places in the Galaxy, but the few differences are informative. An emerging field is the use of nucleosynthesis as a diagnostic of supernova models, both of Type I and II. For example, the synthesis of ^48Ca requires very specific circumstances of low entropy and high neutron excess. The r-process seems to require the conditions that exist in a neutrino driven wind during the first 10 seconds of a neutron star's life. These examples and others will be discussed along with predictions of the masses of black holes and neutron stars to be produced in our Galaxy by Type II supernovae.
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