Physics
Scientific paper
Sep 1993
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993apj...414..717c&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 414, no. 2, p. 717-734.
Physics
24
Hydrodynamics, Neutron Stars, Stellar Evolution, Stellar Interiors, Stellar Mass, Stellar Models, Antineutrinos, Beta Particles, Radioactive Decay, Reaction Kinetics, Stellar Luminosity, Stellar Physics
Scientific paper
The instability of a neutron star at the minimum mass is investigated using a hydrodynamical model to follow the evolution of the unstable star. A detailed analysis of the linear stability of the equilibrium configurations near the minimum mass is performed by solving the radial eigenvalue problem for the fundamental mode. The minimum mass configuration M(mmc) of 0.196 solar mass is found to be stable to small perturbations. Stability to radial perturbations is lost only at a lower critical mass of 0.16 solar mass, corresponding to about 0.8 M(mmc). It is shown that a simple dynamical model constructed using a 3-polytrope equation of state for hot dense matter reproduces the key dynamical features of the instability in the explosion phase.
Colpi Monica
Shapiro Stuart L.
Teukolsky Saul A.
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