Numerical implementation of a perturbation theory up to the third order for rotating polytropic stars - Application to a solar model

Details Numerical implementation of a perturbation theory up to the third order for rotating polytropic stars - Application to a solar model Numerical implementation of a perturbation theory up to the third order for rotating polytropic stars - Application to a solar model

Jun 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986ap%26ss.123..273g&link_type=abstract

Astrophysics and Space Science (ISSN 0004-640X), vol. 123, no. 2, June 1986, p. 273-295.

Statistics

Computation

7

Computational Astrophysics, Perturbation Theory, Polytropic Processes, Solar Rotation, Stellar Models, Stellar Rotation, Stellar Structure

Scientific paper

Numerical treatment of a perturbation theory up to the third order yields quantitative estimates for an interesting polytropic solar model possessing differential rotation of Clement's type. A suitably defined `reduction factor', otherwise referred to as `strength', moderates the effects of the differential rotation and the so resulting limiting state represents efficiently uniform rotation of the model. The numerical results obtained are compared to respective ones derived from an original numerical implementation of a second-order perturbation theory

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