43 research outputs found
Excitation of a nonradial mode in a millisecond X-ray pulsar XTE J1751-305
We discuss candidates for non-radial modes excited in a mass accreting and
rapidly rotating neutron star to explain the coherent frequency identified in
the light curves of a millisecond X-ray pulsar XTE J1751-305. The spin
frequency of the pulsar is Hz and the identified
coherent frequency is . Assuming
the frequency identified is that observed in the corotating frame of the
neutron star, we find that the surface -modes of and 2
excited by -mechanism due to helium burning in the thin shell can
give the frequency ratio at
Hz. As another candidate for the observed ratio ,
we also suggest a toroidal crustal mode that has penetrating amplitudes in the
fluid core and is destabilized by gravitational wave emission.
Since the surface fluid layer is separated from the fluid core by a solid
crust, the amplitudes of an -mode in the core, which is destabilized by
emitting gravitational waves, can be by a large factor different from those in
the fluid ocean. We find that the amplification factor defined as is as large as for the -mode at Hz for a
neutron star model. Because of this significant amplification of
the -mode amplitudes in the surface fluid layer, we suggest that, when
proper corrections to the -mode frequency such as due to the general
relativistic effects are taken into consideration, the core -mode of
can be a candidate for the detected frequency, without leading
to serious contradictions to, for example, the spin evolution of the underlying
neutron star.Comment: 7 pages, 5 figure
R modes of slowly pulsating B stars
We examine pulsational stability of low modes in SPB stars by
calculating fully nonadiabatic oscillations of uniformly rotating stars, where
is an integer representing the azimuthal wave number around the rotation
axis. modes are rotationally induced, non-axisymmetric, oscillation modes,
whose oscillation frequency strongly depends on the rotation frequency
of the star. They are conveniently classified by using two integer indices
and that define the asymptotic oscillation frequency
in the limit of . We find low
, high radial order, odd modes with in SPB stars are
excited by the same iron opacity bump mechanism that excites low frequency
modes of the variables, when the rotation frequency is sufficiently
high. No even modes with low are found to be pulsationally unstable.
Since the surface pattern of the temperature perturbation of odd modes is
antisymmetric about the equator of the star, observed photometric amplitudes
caused by the unstable odd modes with are strongly dependent
on the inclination angle between the axis of rotation and the line of sight.
Applying the wave-meanflow interaction formalism to nonadiabatic modes in
rapidly rotating SPB models, we find that because of the component of
the Reynolds stress and the radial transport of the eddy fluctuation of density
in the rotating star, the surface rotation is accelerated by the forcing due to
the low unstable modes.Comment: submitted to m