2024/01/25 by Hao Tong, Tong, H.
Earth and Planetary Sciences · Engineering · Physics and Astronomy · #FOS: Physical sciences #Geophysics and Sensor Technology #High Energy Astrophysical Phenomena (astro-ph.HE) #High-pressure geophysics and materials #Pulsars and Gravitational Waves Research
paper · pdf · doi:10.48550/arxiv.2401.14157
openalex publication_date 2024/01/25 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
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 105--106 \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.