Dynamical OneArmed Spiral Instability in Differentially Rotating Stars
Abstract
We investigate the dynamical onearmed spiral instability in differentially rotating stars with both eigenmode analysis and hydrodynamic simulations in Newtonian gravity. We find that the onearmed 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 onearmed 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.
 Publication:

22nd Texas Symposium on Relativistic Astrophysics
 Pub Date:
 2005
 arXiv:
 arXiv:astroph/0504002
 Bibcode:
 2005tsra.conf..404S
 Keywords:

 Astrophysics;
 General Relativity and Quantum Cosmology
 EPrint:
 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)