Pulsations of rapidly rotating stellar models based on the Self-Consistent-Field method: numerical aspects and accuracy

Details Pulsations of rapidly rotating stellar models based on the Self-Consistent-Field method: numerical aspects and accuracy Pulsations of rapidly rotating stellar models based on the Self-Consistent-Field method: numerical aspects and accuracy

Nov 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008sf2a.conf..531r&link_type=abstract

"SF2A-2008: Proceedings of the Annual meeting of the French Society of Astronomy and Astrophysics Eds.: C. Charbonnel, F. Combes

Astronomy and Astrophysics

Astrophysics

Scientific paper

We use the numerical method developed in tet{Lignieres2006} and tet{Reese2006} to calculate pulsation modes in stellar models generated by the Self-Consistent-Field method described in tet{Jackson2005} and tet{MacGregor2007}. A discussion on the numerical method and its accuracy is given, followed by a very brief description of some of the results.

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