Phase Transition Between superfluid and Normal states of Neutrons in Neutron Stars--The Origin of Glitches of Pulsars

Simple item page
dc.creatorPeng, Q. H.
dc.creatorLuo, Z. Q.
dc.date2005-01-07
dc.date.accessioned2026-07-07T02:16:40Z
dc.date.available2026-07-07T02:16:40Z
dc.descriptionStarting from a neutron star heating mechanism by the magnetic dipole radiation from the 3^P_2 neutron superfluid vortices in neutron stars, we propose a neutron phase oscillation model which describes the phase transition between the normal neutron Fermi fluid and the 3^P_2 neutron superfluid vortices at the transition temperature of T_{trans}=(5-6)\times 10^8 K. With this model, we can give qualitative explanation to most of the pulsar glitches observed up to date.
dc.description7 pages
dc.identifierhttps://arxiv.org/abs/astro-ph/0501112
dc.identifierhttp://arxiv.org/abs/astro-ph/0501112
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/8872
dc.subjectAstrophysics
dc.titlePhase Transition Between superfluid and Normal states of Neutrons in Neutron Stars--The Origin of Glitches of Pulsars
dc.typetext

Files

Collections

arXiv