From ultraluminous X-ray pulsar to supermassive neutron star
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arXiv
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| Format: | Preprint |
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2024
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| _version_ | 1866913209204604928 |
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| author | Tong, H. |
| author_facet | Tong, H. |
| contents | 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. |
| format | Preprint |
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arxiv_https___arxiv_org_abs_2401_14157 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | From ultraluminous X-ray pulsar to supermassive neutron star Tong, H. High Energy Astrophysical Phenomena 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. |
| title | From ultraluminous X-ray pulsar to supermassive neutron star |
| topic | High Energy Astrophysical Phenomena |
| url | https://arxiv.org/abs/2401.14157 |