Equilibrium magnetized degenerate stellar configurations

Details Equilibrium magnetized degenerate stellar configurations Equilibrium magnetized degenerate stellar configurations

Dec 1976

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1976azh....53.1218s&link_type=abstract

Astronomicheskii Zhurnal, vol. 53, Nov.-Dec. 1976, p. 1218-1224. In Russian.

Astronomy and Astrophysics

Astronomy

1

Magnetic Stars, Pulsars, Stellar Evolution, Stellar Magnetic Fields, White Dwarf Stars, Chandrasekhar Equation, Electron Energy, Electron Gas, Equations Of State, Stellar Models

Scientific paper

It is shown that if a magnetic white dwarf is formed from a magnetic main-sequence star with conservation of magnetic flux during the compression, its parameters do not differ significantly from those of a nonmagnetic white dwarf. If the magnetic-field strength is close to the stability limit of the star with respect to its dynamical equilibrium, then mass and radius of the stable degenerate configuration noticeably increase.

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