The stability of stars with potential-dependent masses

Details The stability of stars with potential-dependent masses The stability of stars with potential-dependent masses

Oct 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990ap%26ss.172..147m&link_type=abstract

Astrophysics and Space Science (ISSN 0004-640X), vol. 172, no. 1, Oct. 1990, p. 147-153.

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1

Gravitational Collapse, Gravitational Effects, Stellar Mass, Computational Astrophysics, Neutron Stars, Relativistic Theory

Scientific paper

The effective mass of a spherical star-like object is calculated under the assumption that the mass of an object represents a function of the gravitational potential in which it occurs. It is shown that due to this mass-dependence on the gravitational potential, it is not possible that a star of a larger mass than that of a neutron star shrinks to a point singularity. The value of the upper limits to the mass of spherical mass bodies is presented as a function of their radii in a large range of their mass densities.

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