Statistics – Computation
Scientific paper
Apr 1989
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989ap%26ss.154..255k&link_type=abstract
Astrophysics and Space Science (ISSN 0004-640X), vol. 154, no. 2, April 1989, p. 255-269.
Statistics
Computation
5
Angular Momentum, Pre-Main Sequence Stars, Stellar Evolution, Stellar Mass, Stellar Rotation, Computational Astrophysics, Convective Flow, Stellar Envelopes, Stellar Luminosity, Stellar Structure, Stellar Temperature
Scientific paper
The evolutionary behavior of rotating low-mass stars in the mass range 0.2 and 0.9 solar mass has been investigated during the pre-Main-Sequence phase. The angular momentum is conserved locally in radiative regions and totally in convective regions, according to a predetermined angular velocity distribution depending on the structure of the star. As the stars contract toward the zero-age Main Sequence, they spin up under the assumption that the angular momentum is conserved during the evolution of the stars. When the stars have differential rotations, their inner regions rotate faster than the outer regions. The effective temperatures and luminosities of rotating low-mass stars obtained are lower than those of nonrotating stars. They have lower central temperature and density values compared to those of nonrotating stars.
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