Stability loss of low-mass stars under conditions of neutronization

Details Stability loss of low-mass stars under conditions of neutronization Stability loss of low-mass stars under conditions of neutronization

Jun 1975

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1975azh....52..469b&link_type=abstract

Astronomicheskii Zhurnal, vol. 52, May-June 1975, p. 469-480. In Russian.

Astronomy and Astrophysics

Astronomy

9

Gravitational Collapse, Neutrinos, Neutron Stars, Stellar Evolution, Stellar Mass, Celestial Mechanics, Dynamic Stability, Hydrodynamic Equations

Scientific paper

Results are presented for numerical calculations of the final evolutionary stage and the loss of mechanical stability experienced by iron cores of 1.21, 1.4, and 1.7 solar masses. In the calculations, beta-process kinetics was consistently taken into account and the hydrodynamic equations were solved in an approximation of a profiled density distribution according to a polytropic law with an index of 3. It is found that the models with 1.7 and 1.4 solar masses have a distinct moment for loss of mechanical stability and transition to the phase of hydrodynamic collapse. The model with 1.21 solar masses does not have such a moment and evolves smoothly to the collapse phase. It is shown that thermodynamic nonequilibrium in the beta processes plays an important role in the evolution of all the models and that URCA neutrinos contribute substantially to the energy-loss rate. The possibility is considered of forming neutron stars of less than 1 solar mass.

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