期刊
ASTROPHYSICAL JOURNAL
卷 618, 期 1, 页码 L37-L40出版社
IOP PUBLISHING LTD
DOI: 10.1086/427653
关键词
gravitational waves; hydrodynamics; instabilities; stars : neutron; stars : rotation
Recent numerical simulations indicate the presence of dynamical instabilities of the f-mode in differentially rotating stars even at very low values of T/\W\, the ratio of kinetic to potential energy. In this Letter we argue that these may be shear instabilities that occur when the degree of differential rotation exceeds a critical value and when the f-mode develops a corotation point associated with the presence of a continuous spectrum. Our explanation, which is supported by detailed studies of a simple shell model, offers a straightforward way of understanding all of the key features of these instabilities.
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