Nonlinear evolution of the r-modes in neutron stars

被引:90
作者
Lindblom, L [1 ]
Tohline, JE
Vallisneri, M
机构
[1] CALTECH, Pasadena, CA 91125 USA
[2] Louisiana State Univ, Dept Phys & Astron, Baton Rouge, LA 70803 USA
[3] Univ Parma, Grp Collegato Parma, Sezione Milano, Ist Nazl Fis Nucl, I-43100 Parma, Italy
基金
美国国家科学基金会;
关键词
D O I
10.1103/PhysRevLett.86.1152
中图分类号
O4 [物理学];
学科分类号
0702 ;
摘要
The evolution of a neutron-star r-mode driven unstable by gravitational radiation is studied here using numerical solutions of the full nonlinear fluid equations. The dimensionless amplitude of the mode grows to order unity before strong shocks develop which quickly damp the mode. In this simulation the star loses about 40% of its initial angular momentum and 50% of its rotational kinetic energy before the mode is damped. The nonlinear evolution causes the fluid to develop strong differential rotation which is concentrated near the surface and poles of the star.
引用
收藏
页码:1152 / 1155
页数:4
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