Computer Science – Numerical Analysis
Scientific paper
Apr 1975
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1975azh....52..243b&link_type=abstract
Astronomicheskii Zhurnal, vol. 52, Mar.-Apr. 1975, p. 243-254. In Russian.
Computer Science
Numerical Analysis
7
Astronomical Models, Self Consistent Fields, Stellar Rotation, White Dwarf Stars, Angular Velocity, Computer Programming, Numerical Analysis, Polytropic Processes, Stellar Structure
Scientific paper
A variant of the self-consistent method for calculating arbitrarily rotating stellar models is described which is simpler and more direct for computer programming and requires less storage capacity than that proposed by Ostriker and Mark (1968). Parameters are tabulated for the rigidly rotating polytropes with n = 1.5 and 3, and are compared with results obtained by previous authors. It is found that rigid rotation cannot stabilize stars with n greater than 3.05 and that rotating models can exist which are stable against small perturbations and have positive total energies. Critical parameters are calculated for differentially rotating white dwarfs undergoing neutronization, and the mass of a differentially rotating stable white dwarf is shown not to exceed 2 solar masses. It is noted that the possibility of turbulence strongly decreases the probability of observing such stars.
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