Relativistic isentropic stellar models

G. Shaviv*, A. Kovetz

*Corresponding author for this work

Research output: Contribution to journalArticlepeer-review

5 Scopus citations


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{variant}) diagram. Models heavier than 20 M become unstable because of pair creation. Iron photodisintegration causes instability in the mass range between 1.5 M and 20 M. General relativistic effects bring about the onset of instability in models of 1.2-1.5 M 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.

Original languageEnglish
Pages (from-to)416-423
Number of pages8
JournalAstrophysics and Space Science
Issue number3
StatePublished - Jun 1970


Dive into the research topics of 'Relativistic isentropic stellar models'. Together they form a unique fingerprint.

Cite this