Superfluidity in neutron stars. II. After a period jump

Greenstein, G

doi:10.1086/154671

Title: Superfluidity in neutron stars. II. After a period jump

Full Record
Other Related Research

Abstract

This paper describes the response of a superfluid neutron star to a sudden increase in the rotation rate of its crust (to a period jump) and shows how the mass, temperature, and distribution of density with radius within a pulsar can in principle be determined to great accuracy by observations of the subsequent spin-down. Observations of successive jumps in the same pulsar can also yield general information concerning the mechanism producing the jumps.This program cannot now be realized. Detailed models are presented of a jump in the Crab pulsar, none of which successfully reproduce the observations. Qualitative reasons for this failure are given and the particular developments, both observational and theoretical, that are required in order to complete the program described. (AIP)

Authors:: Greenstein, G

Publication Date:: Wed Sep 15 00:00:00 EDT 1976

Research Org.:: Amherst College, Amherst, Massachusetts

OSTI Identifier:: 7350940

Resource Type:: Journal Article

Journal Name:: Astrophys. J.; (United States)

Additional Journal Information:: Journal Volume: 208:3

Country of Publication:: United States

Language:: English

Subject:: 71 CLASSICAL AND QUANTUM MECHANICS, GENERAL PHYSICS; NEUTRON STARS; SUPERFLUIDITY; CRAB NEBULA; HYDRODYNAMICS; PULSARS; SPIN; STAR MODELS; ANGULAR MOMENTUM; COSMIC RADIO SOURCES; FLUID MECHANICS; MATHEMATICAL MODELS; MECHANICS; NEBULAE; PARTICLE PROPERTIES; STARS; SUPERNOVA REMNANTS; 640102* - Astrophysics & Cosmology- Stars & Quasi-Stellar, Radio & X-Ray Sources

Citation Formats


                    Greenstein, G. Superfluidity in neutron stars. II. After a period jump.  United States: N. p., 1976. 
        Web.  doi:10.1086/154671.

Copy to clipboard


                    Greenstein, G. Superfluidity in neutron stars. II. After a period jump.  United States.  https://doi.org/10.1086/154671

Copy to clipboard


                    Greenstein, G. 1976.  
        "Superfluidity in neutron stars. II. After a period jump".  United States.  https://doi.org/10.1086/154671.

Copy to clipboard


                    
@article{osti_7350940,

  title        = {Superfluidity in neutron stars. II. After a period jump},

  author       = {Greenstein, G},

  abstractNote = {This paper describes the response of a superfluid neutron star to a sudden increase in the rotation rate of its crust (to a period jump) and shows how the mass, temperature, and distribution of density with radius within a pulsar can in principle be determined to great accuracy by observations of the subsequent spin-down. Observations of successive jumps in the same pulsar can also yield general information concerning the mechanism producing the jumps.This program cannot now be realized. Detailed models are presented of a jump in the Crab pulsar, none of which successfully reproduce the observations. Qualitative reasons for this failure are given and the particular developments, both observational and theoretical, that are required in order to complete the program described. (AIP)},

  doi          = {10.1086/154671},

  url          = {https://www.osti.gov/biblio/7350940},
  journal      = {Astrophys. J.; (United States)},
number       = ,

  volume       = 208:3,

  place        = {United States},

  year         = {Wed Sep 15 00:00:00 EDT 1976},

  month        = {Wed Sep 15 00:00:00 EDT 1976}

}

Copy to clipboard

Journal Article:

https://doi.org/10.1086/154671

Other availability

Find in Google Scholar

Search WorldCat to find libraries that may hold this journal

Save / Share:

Export Metadata

Save to My Library

Similar records in OSTI.GOV collections:

Crust-breaking by neutron superfluids and the VELA pulsar glitches

Journal Article Ruderman, M - Astrophys. J., v. 203, no. 1, pp. 213-222

Anderson's (1975) suggestion of neutron-superfluid vortex pinning and unpinning in the crust lattice of a neutron star as the origin of pulsar timing noise is combined with existing estimates of the lattice breaking strength and creep. For the Vela pulsar, such models give large sudden jumps in frequency and in slowing-down rates as well as an interval between glitches, all of which are comparable to those observed. The qualitative differences between Vela and Crab glitches can also be understood.
https://doi.org/10.1086/154069
Thermally driven neutron star glitches

Journal Article Link, B; Epstein, R - Astrophysical Journal

We examine the thermal and dynamical response of a neutron star to a sudden perturbation of the inner crust temperature. During the star{close_quote}s evolution, starquakes and other processes may deposit {approx_gt}10{sup 42} ergs, causing significant internal heating and increased frictional coupling between the crust and the more rapidly rotating neutron superfluid the star is expected to contain. Through numerical simulation we study the propagation of the thermal wave created by the energy deposition, the induced motion of the interior superfluid, and the resulting spin evolution of the crust. We find that energy depositions of {approximately}10{sup 40} ergs produce gradual spin-upsmore »« less
https://doi.org/10.1086/176779
Neutron star cooling

Journal Article Maxwell, O - Astrophys. J.; (United States)

In order to study the sensitivity of neutron star cooling to nucleon superfluidity and to discover whether neutron stars can cool quickly enough to satisfy the Crab pulsar blackbody observability constraint in the absence of pion condensates, we have performed cooling calculations within a variety of scenarios using a simple, constant-density model for the neutron star interior. These scenarios involve different contributions to the total luminosity and different combinations of proton and neutron superfluidity. To maximize superfluidity effects on the cooling, superfluid gaps are employed which are the maxima as functions of density for particular effective-mass values. Among the coolingmore »« less
https://doi.org/10.1086/157181
Rapid postglitch spin-up of the superfluid core in pulsars

Journal Article Alpar, M; Langer, S; Sauls, J - Astrophys. J.; (United States)

Vortex lines in the superfluid cores of neutron stars carry flux due to the induced proton charge current which results from the Fermi liquid interaction between neutrons and protons. As a consequence the scatttering of charges off these magnetic vortex lines equilibrates the core superfluid to the plasma and the crust on time scales of order 1 second after a glitch. Thus, the core superfluid cannot be responsible for the observed time scales of the Vela and Crab pulsars. This result supports the theory of Alpar et al, in which both the glitch and the slow postglitch relaxation are determinedmore »« less
https://doi.org/10.1086/162232
Superfluidity in neutron stars. III. Relaxation processes between the superfluid and the crust

Journal Article Harding, D; Guyer, R; Greenstein, G - Astrophys. J.; (United States)

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 previousmore »« less
https://doi.org/10.1086/156217

Similar Records