Asymptotic theory of gravity modes in rotating stars
نویسندگان
چکیده
منابع مشابه
Asymptotic expressions for the angular dependence of low-frequency pulsation modes in rotating stars
Through the solution of Laplace’s tidal equations, approximated to describe equatorially trapped wave propagation, analytical expressions are obtained for the angular dependence of pulsation modes in uniformly rotating stars. As the ratio between rotation and pulsation frequencies becomes large, these expressions approach the exact solutions of the governing low-frequency pulsation equations. F...
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We investigate the effect of a magnetic field on the global oscillation modes of a rotating fluid star in the magnetohydrodynamic approximation. We present general equations for the modification of any type of fluid mode due to a general magnetic field which is not aligned with the star’s spin axis. In the case of any internal dipole magnetic field we derive the equations for the frequency corr...
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We investigate inertial mode oscillations of slowly and uniformly rotating, isentropic, Newtonian stars. Inertial mode oscillations are induced by the Coriolis force due to the star’s rotation, and their characteristic frequencies are comparable with the rotation frequency Ω of the star. So called r-mode oscillations form a sub-class of the inertial modes. In this paper, we use the term “r-mode...
متن کاملAsymptotic analysis of high-frequency acoustic modes in rapidly rotating stars
Context. The asteroseismology of rapidly rotating pulsating stars is hindered by our poor knowledge of the effect of the rotation on the oscillation properties. Aims. Here we present an asymptotic analysis of high-frequency acoustic modes in rapidly rotating stars. Methods. We study the Hamiltonian dynamics of acoustic rays in uniformly rotating polytropic stars and show that the phase space st...
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Gravitational radiation tends to drive gravity modes in rotating neutron stars unstable. For an inviscid star, the instability sets in when the rotation frequency is about 0.7 times the corresponding mode frequency of the nonrotating star. Neutron stars with spin frequencies > ∼ 100 Hz are susceptible to this instability, with growth time of order years. However, it is likely that viscous dissi...
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ژورنال
عنوان ژورنال: Astronomy & Astrophysics
سال: 2016
ISSN: 0004-6361,1432-0746
DOI: 10.1051/0004-6361/201527737