Structure-distortion of polytropic stars by differential rotation - Third-order perturbation theory

Details Structure-distortion of polytropic stars by differential rotation - Third-order perturbation theory Structure-distortion of polytropic stars by differential rotation - Third-order perturbation theory

Jan 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981ap%26ss..74...97g&link_type=abstract

Astrophysics and Space Science, vol. 74, no. 1, Jan. 1981, p. 97-110. Research supported by the University of Patras.

Astronomy and Astrophysics

Astrophysics

16

Perturbation Theory, Polytropic Processes, Rotating Fluids, Stellar Rotation, Stellar Structure, Angular Velocity, Boundary Value Problems, Fortran, Stellar Models

Scientific paper

Chandrasekhar's perturbation theory is extended to include third-order
terms in the perturbation parameter in order to specify the structure of
a rapidly and differentially rotating gaseous polytrope. It is noted
that in order to employ this method in determining the structure of a
polytropic star, a suitable FORTRAN program must be extended.

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