Astronomy and Astrophysics – Astrophysics
Scientific paper
Oct 1975
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1975nyasa.262...47a&link_type=abstract
(AAS, American Physical Society, and New York Academy of Sciences, Texas Symposium on Relativistic Astrophysics, 7th, Dallas, Te
Astronomy and Astrophysics
Astrophysics
13
Electron Capture, Gravitational Collapse, Nuclear Reactions, Stellar Evolution, Electron Density (Concentration), Helium, Hydrodynamics, Neutron Stars, Nucleons, Stellar Mass, Thermodynamic Properties, Velocity Distribution
Scientific paper
Some calculation results are given for two of the near-final stages of massive star evolution, namely, neutronization and nuclear disintegration followed by collapse of central regions. Electron number density is plotted against the corresponding nucleon number. Above a central density of about 40 billion g/cu cm, neutronization is fast, and a balance between electron destruction and replacement does not occur until central density reaches about 300 billion g/cu cm. It is interesting that electron capture always tends to heat the matter. Infall and sound velocities are plotted versus radius for when the central density reaches a trillion g/cu cm. Infall velocities inferior to r equals 10 million cm are quite subsonic, and the material is contracting quasi-hydrostatically as new matter accretes through the neutronizing region. Further out, infall velocity rises to a maximum and a shock front is developing.
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