Two possible approaches to form sub-millisecond pulsars
| dc.creator | Du, Yuanjie | |
| dc.creator | Xu, R. X. | |
| dc.creator | Qiao, G. J. | |
| dc.creator | Han, J. L. | |
| dc.date | 2008-03-10 | |
| dc.date | 2008-11-20 | |
| dc.date.accessioned | 2026-07-07T10:19:18Z | |
| dc.date.available | 2026-07-07T10:19:18Z | |
| dc.description | Pulsars have been recognized as normal neutron stars or quark stars. Sub-millisecond pulsars, if detected, would play an essential and important role in distinguishing quark stars from neutron stars. A key question is how sub-millisecond pulsars could form. Both sub-Keplerian (for neutron and quark stars) and super-Keplerian cases (only for quark stars, which are bound additionally by strong interaction) have been discussed in this paper in order to investigate possible ways of forming sub-millisecond pulsars. In the sub-Keplerian case, the equilibrium periods of both neutron and quark stars could be as low as ~0.4 ms when they are spun up through accretion in binary systems. In the super-Keplerian case, pulsars could very likely have an initial period of ~0.1 ms if quark stars with different mass could be formed from accretion-induced collapse (AIC) of white dwarfs. The timescale for a sub-millisecond pulsar to keep its period <1 ms is restricted due to gravitational wave radiation. We found that the timescales of neutron stars within sub-millisecond periods are approximately ~10 yr, but the timescales estimated (>10 Myr) for low-mass quark stars could be long enough for us to detect. | |
| dc.description | 12pages, 1 figure, 3 table, this paper has been withdrawn | |
| dc.identifier | https://arxiv.org/abs/0803.1334 | |
| dc.identifier | http://arxiv.org/abs/0803.1334 | |
| dc.identifier.uri | http://salesiana.dossiersoluciones.com/handle/123456789/174463 | |
| dc.subject | Astrophysics | |
| dc.title | Two possible approaches to form sub-millisecond pulsars | |
| dc.type | text |