Statistics – Computation
Scientific paper
Aug 1979
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979azh....56..770b&link_type=abstract
Astronomicheskii Zhurnal, vol. 56, July-Aug. 1979, p. 770-780. In Russian.
Statistics
Computation
1
Gravitational Collapse, Stellar Evolution, Stellar Rotation, Angular Momentum, Stellar Mass, Velocity Distribution
Scientific paper
The evolution of rapidly rotating stars in the stage of gravitational contraction is calculated by using a rigorous technique based on the self-consistent field method to determine the structure of models of such stars with a convective core and radiative envelope. Rotation laws for convective cores are considered, and a law of uniform rotation is adopted. Computational results are presented for stars of 0.5, 1, 2, and 10 solar masses, as well as for different angular momenta on the assumption that angular momentum is conserved during evolution. For low-mass stars (0.5 and 1 solar mass) the technique employed is found to be valid almost up to the time when the main sequence is reached, which makes it possible to estimate the increase in time of approach to the main sequence due to rotation. It is shown that this time approximately doubles for the maximum values of angular momentum.
Bisnovatyi-Kogan Gennadi S.
Blinnikov Sergei I.
Fedorova Alexandra V.
Kostiuk N. D.
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