Stellar stability in Newtonian theory of gravitation with shadow effect

Details Stellar stability in Newtonian theory of gravitation with shadow effect Stellar stability in Newtonian theory of gravitation with shadow effect

Dec 1975

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1975ncimb..30..280c&link_type=abstract

Nuovo Cimento, Sezione B, vol. 30 B, Dec. 11, 1975, p. 280-290.

Astronomy and Astrophysics

Astrophysics

2

Field Theory (Physics), Gravitation Theory, Newton Theory, Relativity, Stellar Gravitation, Astronomical Models, Astrophysics, Equilibrium Equations, Hydrostatics, Mass Distribution, Quantum Theory, Secular Variations, Shadows, Stellar Mass, Variational Principles

Scientific paper

The Newtonian theory of gravitation with shadow effect is applied to discuss the conditions for hydrostatic equilibrium and stability of stellar models. In particular, a uniform-density spherical star model is analyzed in some detail. It is found that the critical adiabatic index for stability is always smaller than 4/3, in contrast to what happens in ordinary Newtonian theory. Possible generalizations of the theory as well as its applications in astrophysics are briefly indicated.

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