Relativistic Isentropic Stellar Methods

Details Relativistic Isentropic Stellar Methods Relativistic Isentropic Stellar Methods

Jun 1970

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1970ap%26ss...7..416s&link_type=abstract

Astrophysics and Space Science, Volume 7, Issue 3, pp.416-423

Astronomy and Astrophysics

Astrophysics

3

Scientific paper

Relativistic, isentropic, homogeneous models are constructed by a method that automatically detects instabilities, and evolutionary tracks of central conditions are shown on a (T, ϱ) diagram. Models heavier than 20M &sun; become unstable because of pair creation. Iron photodisintegration causes instability in the mass range between 1.5M &sun; and 20M &sun;. General relativistic effects bring about the onset of instability in models of 1.2 1.5M &sun; when the central density is about 1010 g/cm3. Lighter models become white dwarfs. It is pointed out that general relativistic instability will prevent the formation of neutron stars through hydrostatic evolution and may be relevant in setting off low-mass supernovae.

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