From ultraluminous X-ray pulsar to supermassive neutron star

The formation of a $2.7{\mathrm{M}}_{\odot }$ 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 ${10}^5$–${10}^6\mathrm{y}\mathrm{r}$. 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.