Superfluidity in neutron stars. III. Relaxation processes between the superfluid and the crust
We calculate the rates for a variety of processes whereby the neutron superfluid within a neutron star exchanges momentum with the charged-particle system with which it coexists. We consider the scattering of the normal neutron fluid within vortex lines from phonons (one- and two-phonon processes) impurities and lattice defects in the crust, and momentum transfer brought about by neutron ..beta..-decay. We neglect vortex pinning, and confine attention to the regime of isotropic superfluidity: that is, for that portion of the superfluid tha coexists with the crust.We then turn to a discussion of the ways in which the results of previous hydrodynamical calculations are altered by our new relaxation rates. Of particular interest is a major discrepancy between the predicted and the observed spin-down of a pulsar after a period jump, a discrepancy that can be resolved by proposing that neutron stars are bigger than has been previously thought.
- Research Organization:
- Department of Physics and Astronomy, University of Massachusetts, Amherst
- OSTI ID:
- 6674775
- Journal Information:
- Astrophys. J.; (United States), Vol. 222:3
- Country of Publication:
- United States
- Language:
- English
Similar Records
Superfluid Friction and Late-Time Thermal Evolution of Neutron Stars
Thermally activated post-glitch response of the neutron star inner crust and core. I. Theory
Related Subjects
GENERAL PHYSICS
NEUTRON STARS
SUPERFLUIDITY
BETA DECAY
HAMILTONIANS
NEUTRONS
NUCLEAR REACTIONS
PHONONS
SCATTERING
SPECTRAL FUNCTIONS
UMKLAPP PROCESSES
VORTEX FLOW
BARYONS
BASIC INTERACTIONS
DECAY
ELECTROMAGNETIC INTERACTIONS
ELEMENTARY PARTICLES
FERMIONS
FLUID FLOW
FUNCTIONS
HADRONS
INTERACTIONS
LEPTONIC DECAY
MATHEMATICAL OPERATORS
NUCLEONS
PARTICLE DECAY
QUANTUM OPERATORS
QUASI PARTICLES
STARS
WEAK INTERACTIONS
WEAK PARTICLE DECAY
640102* - Astrophysics & Cosmology- Stars & Quasi-Stellar
Radio & X-Ray Sources