The Magnetic Field in the Stability of the Stars

Angel Fierros Palacios^*

Instituto de Investigaciones Eléctricas, División de Energías Alternas, Mexico City, México.

DOI: 10.4236/jhepgc.2015.12008                

Abstract

The theoretical frame developed by A. S. Eddington is used in this paper in order to study the problem of internal structure and stars stability. A new hypothesis is developed that consists of assuming that at early stage of their evolution, all gaseous stars generate an intense magnetic field whose mission is to contribute to their stability. A simple methodology is shown to calculate the magnitude of the self-generated magnetic field at any point of the star, and diagrams are built for two specific cases, where the way in which this field varies from the center to the surface can be seen. Finally, the problem of the Cepheid type variables is studied obtaining an expression for the oscillation period carried out from the differential equation of the simple harmonic movement in terms of the appropriate parameters of the star.

Keywords

Structure of Stars, Stability of the Stars, Cepheid Variables

Conflicts of Interest

The authors declare no conflicts of interest.

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