Microscopic magnetic dipole radiation in neutron stars

Abstract

There is ${}^3{P}_2$ neutron superfluid region in NS (neutron star) interior. For a rotating NS, the ${}^3{P}_2$ superfluid region is like a system of rotating magnetic dipoles. It will give out electromagnetic radiation, which may provides a new heating mechanism of NSs. This heating mechanism plus some cooling agent may give sound explanation to NS glitches.

To be published by ChJAA

References in corpus (10)

• Neutrino Emission from Neutron Stars
• Minimal Cooling of Neutron Stars: A New Paradigm
• The Cooling of Compact Stars
• Deviations from Chemical Equilibrium due to Spin-Down as an Internal Heat Source in Neutron Stars
• Enhanced cooling of neutron stars via Cooper-pairing neutrino emission
• Superfluidity in beta-stable neutron star matter
• What we can learn from observations of cooling neutron stars
• Rotochemical Heating of Neutron Stars: Rigorous Formalism with Electrostatic Potential Perturbations
• Thermal evolution of rotating hybrid stars
• Improbability of DUrca process constraints EOS

Cited by in corpus (2)

• Resonant cyclotron scattering in pulsar magnetospheres and its application to isolated neutron stars
• The optical/UV excess of isolated neutron stars in the RCS model