Models of magnetic white dwarfs.
Abstract
This paper is devoted to the effects brought by the presence of a strong internal magnetic field on the structure of white dwarfs. The spherical equations of hydrostatic equilibrium are solved by using the following approximation: the actual magnetic pressure is replaced by its radial component averaged over a spherical shell. Physically, this represents the case in which the field lines within the star are severely twisted. Using adequate hypothesis about the behavior of the field strength, the net force due to the field is then approximately radial. Comparisons with the model of Ostriker and Hartwick (1968) are made and show an excellent agreement. The effects of electrostatic corrections to cold electron pressure, of betainverse decays and of pycnonuclear reactions have also been considered. Massradius relationships are given for various values of the ratio of the magnetic energy to the gravitational energy of the white dwarf, and for various values of the highest excited Landau level.
 Publication:

Astronomy and Astrophysics
 Pub Date:
 May 1986
 Bibcode:
 1986A&A...160...95A
 Keywords:

 Magnetic Effects;
 Stellar Magnetic Fields;
 Stellar Models;
 Stellar Structure;
 White Dwarf Stars;
 Chandrasekhar Equation;
 Magnetic Field Configurations;
 Magnetohydrodynamic Stability;
 Stellar Mass;
 Astrophysics