Excitation of a nonradial mode in a millisecond X-ray pulsar XTE J1751-305

Abstract

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 ${\nu }_{\mathrm{spin}}\cong 435$Hz and the identified coherent frequency is ${\nu }_{\mathrm{osc}}=0.5727595\times {\nu }_{\mathrm{spin}}$. Assuming the frequency identified is that observed in the corotating frame of the neutron star, we find that the surface $r$-modes of $l^{\prime }=m=1$ and 2 excited by $\epsilon$-mechanism due to helium burning in the thin shell can give the frequency ratio $\kappa ={\nu }_{\mathrm{osc}}/{\nu }_{\mathrm{spin}}\simeq 0.57$ at ${\nu }_{\mathrm{spin}}=435$Hz. As another candidate for the observed ratio $\kappa$, 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 $r$-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 $f_{\mathrm{amp}}={\alpha }_{\mathrm{surface}}/{\alpha }_{\mathrm{core}}$ is as large as $f_{\mathrm{amp}}\sim 10^2$ for the $l^{\prime }=m=2$ $r$-mode at ${\nu }_{\mathrm{spin}}=435$Hz for a $M=1.4M_{\odot }$ neutron star model. Because of this significant amplification of the $r$-mode amplitudes in the surface fluid layer, we suggest that, when proper corrections to the $r$-mode frequency such as due to the general relativistic effects are taken into consideration, the core $r$-mode of $l^{\prime }=m=2$ can be a candidate for the detected frequency, without leading to serious contradictions to, for example, the spin evolution of the underlying neutron star.

7 pages, 5 figures

References in corpus (1)

• Axisymmetric toroidal modes of magnetized neutron stars

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