Hostname: page-component-7b7567c8c-lpg2g Total loading time: 0 Render date: 2026-11-15T17:56:19.685Z Has data issue: false hasContentIssue false

White Dwarf Rotation: Observations and Theory

Published online by Cambridge University Press:  26 May 2016

Steven D. Kawaler*
Affiliation:
Department of Physics and Astronomy, Iowa State University, Ames, IA 50011 USA

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the 'Save PDF' action button.

White dwarfs rotate. The angular momentum in single white dwarfs must originate early in the life of the star, but also must be modified (and perhaps severely modified) during the many stages of evolution between birth as a main–sequence star and final appearance as a white dwarf. Observational constraints on the rotation of single white dwarf stars come from traditional spectroscopy and from asteroseismology, with the latter providing hints of angular velocity with depth. Results of these observational determinations, that white dwarfs rotate with periods ranging from hours to days (or longer), tells us that the processes by which angular momentum is deposited and/or drained from the cores of AGB stars are complex. Still, one can place strong limits on these processes by considering relatively simple limiting cases for angular momentum evolution in prior stages, and on subsequent angular momentum evolution in the white dwarfs. These limiting-case constraints will be reviewed in the context of the available observations.

Information

Type
Session 5 Final Stages, Nucleosynthesis
Copyright
Copyright © Astronomical Society of the Pacific 2004