On the Evolution of a Rotationally Unstable Star

Publisher Website
Google Scholar
Abstract
The fission theory of binary star systems is reexamined and important objections to it are removed. The presence of a magnetic field in the atmosphere of a rotationally unstable star prevents loss of momentum through the loss of atmosphere at the star's equator. By interaction with the atmospheric electric and magnetic fields, the ions are constrained to move systematically in the direction of rotation and add angular momentum to the star proper. Eventually the star divides, and whereas the parent star was radially symmetrical the resulting components are highly asymmetrical and one-half of the star is at a much higher mean temperature than the other half. Tidal couples orient the components just after fission so that the newly exposed faces are oriented inward but are displaced through a small angle. The comparatively high temperatures of the hot faces cause the star to lose mass asymmetrically by radiation or by loss of atmosphere.

This publication has 7 references indexed in Scilit: