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

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

2005-01-07

arxiv.org/abs/astro-ph/0501112v1

Astronomy and Astrophysics

Astrophysics

7 pages

Scientific paper

Starting 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.

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