Rotating Stars with Very Large Magnetic Fields

Open Access
Publisher Website
Google Scholar
Abstract
Uniformly rotating main sequence stars with strong dipole magnetic fields are examined using a perturbation method. The spherically symmetric part of the perturbing forces is taken into account essentially exactly, while the non-spherical terms are treated as a perturbation. The form of the internal magnetic field, the perturbations to the pressure, temperature, luminosity and the surface are computed. With a strong magnetic field alone the total luminosity is reduced, the non-spherical contribution to the luminosity is positive at the pole and negative at the equator. The non-spherical contribution to the temperature is negative at the pole and positive at the equator. The surface of the star is doughnut shaped and lies within the surface of the star without a magnetic field.

This publication has 0 references indexed in Scilit: