An implicit stellar evolution code, with an application to main-sequence evolution

Details An implicit stellar evolution code, with an application to main-sequence evolution An implicit stellar evolution code, with an application to main-sequence evolution

Jan 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987a%26a...171...87v&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 171, no. 1-2, Jan. 1987, p. 87-94. ZWO-supported research.

Astronomy and Astrophysics

Astrophysics

1

Computer Programs, Convective Heat Transfer, Main Sequence Stars, Stellar Composition, Stellar Evolution, Stellar Models, Density Distribution, Hertzsprung-Russell Diagram, Stellar Mass, Stellar Temperature

Scientific paper

A description is given of a new program for the computation of evolutionary sequences of stellar models with consistent and very precise composition profiles. A completely implicit method is used for solving the chemical composition and the location of convective boundaries. Details of the input physics are presented. An application is presented to the calculation of evolutionary sequences for stars with masses of 1, 1.5, 2, 3, 4, 6, 9, 16,20, 30 Msun (X=0.70; Z=0.03) from the zero-age main sequence through hydrogen shell burning. Also a grid of homogeneous Zero Age Main Sequence models is computed for X=0.70; Z= , 10-5, 10-4, 10-3, 10-2, 0.03. For Z=0.03 the models cover the mass range 0.2 < M/Msun < 200, for the other Z-values the range is 1 < M/Msun < 40. A comparison with results of other authors (notably Becker, 1981; and Alcock and Paczynski, 1980) shows in general a very satisfactory agreement.

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