New radiative opacities: Their influence on stellar models

Details New radiative opacities: Their influence on stellar models New radiative opacities: Their influence on stellar models

Feb 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994a%26a...282..760c&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 282, no. 3, p. 760-765

Astronomy and Astrophysics

Astrophysics

13

Opacity, Stellar Evolution, Stellar Interiors, Stellar Models, Stellar Structure, Helium, Hydrogen, Mathematical Models, Metallicity, Stellar Composition, Stellar Mass, Thermonuclear Reactions

Scientific paper

We investigate the influence of different assumptions about radiative opacity on the theoretical evolution of stellar structures in the range of low and intermediate mass stars. Selected evolutionary models with Z less than or = 0.02 have been evolved through H and He burning phases, in order to allow a comparison between models obtained on the basis of either the recent Livermore (OPAL) or the previous Los Alamos opacity tabulations (LAOL). Our main results are: (1) The use of OPAL produce appreciable variations of the evolutionary scenario only for stellar models having mass larger than 3 solar mass (at Z = 0.02). (2) In all cases, stellar properties depending on the physical structure of the H or He burning cores are practically insensitive to the latest opacity computations. In particular, this is the case for lifetimes during both H and He burning phases. (3) When a stellar model presents an extended radiative envelope (as for example during most of the central He burning of an intermediate mass stars) the use of the OPAL leads to significantly more faint models. This difference between models produced by means of new and old opacity decreases as the metallicity is decreased. (4) Such differences can be largely eliminated by moderately increasing the true metallicity of LAOL models with respect to their nominal values.

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