Computer Science – Numerical Analysis
Scientific paper
Jan 1994
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994apj...420..880k&link_type=abstract
The Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 420, no. 2, p. 880-883
Computer Science
Numerical Analysis
20
Cepheid Variables, Globular Clusters, Numerical Analysis, Stellar Interiors, Stellar Models, Stellar Oscillations, Abundance, Fine Structure, Stellar Evolution, Stellar Mass
Scientific paper
Comparative linear nonadiabatic pulsation calculations are presented using the OPAL and Opacity Project opacities. The two sets of opacities include effects due to intermediate coupling and fine structure as well as new abundances. We used two mass luminosity (M-L) relations, one standard (BIT), and one employing substantial convective core overshoot (COV). The two sets of opacities cannot be differentiated on the basis of the stellar pulsation calculations presented here. The BIT relation can model the beat and bump Cepheids with masses between 4 and 7 solar mass, while if the overshoot relation is used, masses between 2 and 6 solar mass are required. In the RR Lyrae regime, we find the inferred masses of globular cluster RRd stars to be little influenced by the choice of OPAL or OP. Finally, the limited modeling we have done is not able to constrain the Cepheid M-L relation based upon period ratios observed in the beat and bump stars.
Kanbur Shashi M.
Simon Norman R.
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