From ultraluminous X-ray pulsar to supermassive neutron star

H. Tong

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arXiv · 2401.14157

From ultraluminous X-ray pulsar to supermassive neutron star

H. Tong

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Abstract

The formation of a $2.7\ \rm M_{\odot}$ supermassive neutron star is explored, as the possible companion of PSR J0514--4002E. Magnetars may experience super-Eddington accretion. Observationally they may manifest themselves as ultraluminous X-ray pulsars. We propose that supermassive neutron stars may be formed through ultraluminous X-ray pulsar phase, if the ultraluminous X-ray pulsar phase can last for $10^{5}$--$10^6 \ \rm yr$. The accreted material will also bury the magnetic field of the neutron star. Assuming accretion equilibrium, the final output may be a millisecond supermassive neutron star. In order for the ultraluminous X-ray pulsar phase to last long enough, a magnetic field configuration of the low magnetic field magnetar is required. The mass, magnetic field and rotational evolution of super-Eddington accreting neutron stars are rather robust against different assumptions, although many of the model details are yet to be determined.

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H. Tong. 2024-01-25. From ultraluminous X-ray pulsar to supermassive neutron star. https://arxiv.org/abs/2401.14157

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