On stellar models with an isothermal core in the presence of a magnetic field
Abstract
The effect of a poloidal magnetic field on stellar models with nondegenerate isothermal cores and envelopes in either radiative or convective equilibrium has been investigated using a perturbation technique. It is shown that, for models with radiative envelopes, the presence of a magnetic field tends to reduce the maximum limit on the core mass fraction (ratio of core mass to the total mass). In the case of models with convective envelopes, for a given strength of the magnetic field, the maximum mass of the composite star is reached at a critical value of the central density which is higher than the corresponding nonmagnetic case. Using an unrestricted secondorder virial tensor method, the effect of a magnetic field on the dynamical stability of these models is investigated. It has been shown that the magnetic field induces stability in the models by shifting the point of critical stability to a higher value of central density.
 Publication:

The Astrophysical Journal
 Pub Date:
 June 1984
 DOI:
 10.1086/162099
 Bibcode:
 1984ApJ...281..292D
 Keywords:

 Magnetic Stars;
 Stellar Cores;
 Stellar Magnetic Fields;
 Stellar Models;
 Dynamic Stability;
 Isothermal Processes;
 Poloidal Flux;
 Polytropic Processes;
 Stellar Envelopes;
 Stellar Evolution;
 Stellar Mass;
 Stellar Oscillations;
 Stellar Structure;
 Astrophysics