Phase Transition in Pulsar Timing
| dc.creator | Glendenning, Norman K. | |
| dc.date | 1998-03-06 | |
| dc.date.accessioned | 2026-07-07T02:26:18Z | |
| dc.date.available | 2026-07-07T02:26:18Z | |
| dc.description | A phase transition in the nature of matter in the core of a neutron star, such as quark deconfinement or Bose condensation, can cause the spontaneous spin-up of a solitary millisecond pulsar. The spin-up epoch for our model lasts for $2\times 10^7$ years or 1/50 of the spin-down time (Glendenning, Pei and Weber in Ref. \cite{glen97:a}). The possibility exists also for future measurements on X-ray neutron stars with low-mass companions for mapping out the tell-tale ``backbending'' behavior of the moment of inertia. Properties of phase transitions in substances such as neutron star matter, which have more than one conserved charge, are reviewed. | |
| dc.description | 18 pages, 9 figures, Latex. (Invited Paper, Hirschegg '98, Nuclear Astrophysics, Organizers: M. Buballa, W. Norenberg, J. Wambach and A.\ Wirzba) | |
| dc.identifier | https://arxiv.org/abs/astro-ph/9803074 | |
| dc.identifier | http://arxiv.org/abs/astro-ph/9803074 | |
| dc.identifier.uri | http://salesiana.dossiersoluciones.com/handle/123456789/12220 | |
| dc.subject | Astrophysics | |
| dc.subject | Nuclear Theory | |
| dc.title | Phase Transition in Pulsar Timing | |
| dc.type | text |