Construction of internal-structure models for stars at the beginning of the main sequence

Details Construction of internal-structure models for stars at the beginning of the main sequence Construction of internal-structure models for stars at the beginning of the main sequence

Jun 1974

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1974urbar..59...17a&link_type=abstract

Urania (Madrid), vol. 59, Jan.- June 1974, p. 17-35. In Spanish.

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Computation

Astronomical Models, Main Sequence Stars, Mathematical Models, Stellar Evolution, Stellar Interiors, Stellar Mass, Stellar Structure, Chemical Composition, Differential Equations, Radiation Pressure, Radiative Transfer, Tables (Data), Thermal Stability

Scientific paper

A description is given of a computational method for the design of theoretical static models of the internal structure of stars belonging to population I, taking into account stars which are in the initial evolutionary stage of the main sequence. The stellar mass of the stars considered is in the range from 1.7 to 20 solar masses. The computations presented have been undertaken for a star with a mass corresponding to 8 solar masses. This selection makes it possible to obtain sufficient observational data for an evaluation of the theoretical results.

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