Dynamical One-Armed Spiral Instability in Differentially Rotating Stars
Abstract
We investigate the dynamical one-armed spiral instability in differentially rotating stars with both eigenmode analysis and hydrodynamic simulations in Newtonian gravity. We find that the one-armed spiral mode is generated around the corotation radius of the star, and the distribution of angular momentum shifts inwards the corotation radius during the growth of one-armed spiral mode. We also find by investigating the distribution of the canonical angular momentum density that the low T/|W| dynamical instability for both m=1 and m=2 mode, where T is the rotational kinetic energy and W is the gravitational potential energy, is generated around the corotation point. Finally, we discuss the feature of gravitational waves generated from these modes.
Cite
@article{arxiv.astro-ph/0504002,
title = {Dynamical One-Armed Spiral Instability in Differentially Rotating Stars},
author = {Motoyuki Saijo and Shin'ichirou Yoshida},
journal= {arXiv preprint arXiv:astro-ph/0504002},
year = {2007}
}
Comments
6 pages with 6 eps figures, revsymb.sty. To appear in Proceedings of the 22nd Texas Symposium on Relativistic Astrophysics, Stanford, 2004, edited by P. Chen (SLAC Electronic Conference Proceedings)