Statistics – Computation
Scientific paper
Feb 1994
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994rspta.346..251b&link_type=abstract
Philosophical Transactions: Physical Sciences and Engineering, Volume 346, Issue 1680, pp. 251-258
Statistics
Computation
3
Scientific paper
Supernovae of type II happen at the end of the evolution of massive stars, 10 times the mass of the Sun, [Note: See the image of page 251 for this formatted text] MO, or more. To begin with, the central core, of mass about [Note: See the image of page 251 for this formatted text] 1.5 MO, collapses; the large gravitational energy remains for a while in the core. It is then released in the form of neutrinos. A small fraction, 1 or 2%, of the neutrino energy is absorbed in the mantle of the star, i.e. the region 100 or 500 km from the centre; this drives the shock. It is essential that vigorous convection occurs in the shocked material. With reasonable assumptions, one can estimate the energy in the shock to be of the order 1051 erg, in agreement with observation. The argument is based on observation and analytical calculations, with a minimum of help from elaborate computations.
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