Perturbation method for the structure of slowly rotating stars.

Details Perturbation method for the structure of slowly rotating stars. Perturbation method for the structure of slowly rotating stars.

Sep 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996acasn..37..254w&link_type=abstract

Acta Astron. Sin., Vol. 37, No. 3, p. 254 - 266

Astronomy and Astrophysics

Astronomy

1

Neutron Stars: Rotation, Neutron Stars: Equation Of State

Scientific paper

The authors used the perturbation method to solve stationary axially symmetric stellar equilibrium configuration slowly rotating with uniform angular velocity in the framework of general relativity. The structure equation used are the full relativistic equations expand in powers of the angular velocity Ω, neglecting terms greater than orders of Ω2. They calculated the structures of stable configuration based on 10 different possible equations of state for neutron stars. Through the calculation results based on EOS G, they discussed the details of the effects of rotation on the stellar structure and properties of the neutron stars.

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