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Article: Postglitch relaxation of the vela pulsar after its first eight large glitches: A reevaluation with the vortex creep model

TitlePostglitch relaxation of the vela pulsar after its first eight large glitches: A reevaluation with the vortex creep model
Authors
KeywordsDense Matter
Pulsars: Individual (Vela)
Stars: Neutron
Issue Date1993
PublisherInstitute of Physics Publishing Ltd. The Journal's web site is located at http://iopscience.iop.org/2041-8205
Citation
Astrophysical Journal Letters, 1993, v. 409 n. 1, p. 345-359 How to Cite?
AbstractWe present a comprehensive reevaluation of eight of the nine glitches observed to date from the Vela pulsar, and the postglitch relaxation following each glitch. All glitch data sets can be described in terms of three distinct components of short and intermediate time scale exponential relaxation, followed by a long-term recovery of the glitch-induced change in the spin-down rate that is linear in t, ΔΩ̇ c(t) ∝ t. We interpret the short and the intermediate time scale exponential relaxation, characterized by relaxation times of 10 hr, 3 d.2, and 32 d as the linear response of vortex creep in those regions of the pinned superfluid in the neutron star crust through which no sudden vortex motion occurred at the time of the glitch. The long-term recovery is interpreted as the nonlinear response of vortex creep regions. In addition, there are regions of the crustal superfluid which cannot sustain a vortex density or vortex creep current, but which play a significant role in determining the angular momentum balance. The tendency of glitches to leave permanent spin-up remnants is explained as a discrete internal torque which in glitches, couples part of the crustal superfluid to the observed crust. We find that, on average, the theoretically expected interglitch intervals agree quite well with the observed intervals. The same set of short and intermediate relaxation times, with similar values of moments of inertia for the various components of the crustal superfluid, yield good fits for all postglitch data sets. Furthermore, these relaxation times and moments of inertia are compatible with previous theoretical estimates. A moment of inertia fraction of at least 0.024 is implied for the crustal superfluid. This result rules out neutron star models based on soft equations of state.
Persistent Identifierhttp://hdl.handle.net/10722/174911
ISSN
2015 Impact Factor: 5.487
2015 SCImago Journal Rankings: 3.369

 

DC FieldValueLanguage
dc.contributor.authorAli Alpar, Men_US
dc.contributor.authorChau, HFen_US
dc.contributor.authorCheng, KSen_US
dc.contributor.authorPines, Den_US
dc.date.accessioned2012-11-26T08:48:05Z-
dc.date.available2012-11-26T08:48:05Z-
dc.date.issued1993en_US
dc.identifier.citationAstrophysical Journal Letters, 1993, v. 409 n. 1, p. 345-359en_US
dc.identifier.issn2041-8205en_US
dc.identifier.urihttp://hdl.handle.net/10722/174911-
dc.description.abstractWe present a comprehensive reevaluation of eight of the nine glitches observed to date from the Vela pulsar, and the postglitch relaxation following each glitch. All glitch data sets can be described in terms of three distinct components of short and intermediate time scale exponential relaxation, followed by a long-term recovery of the glitch-induced change in the spin-down rate that is linear in t, ΔΩ̇ c(t) ∝ t. We interpret the short and the intermediate time scale exponential relaxation, characterized by relaxation times of 10 hr, 3 d.2, and 32 d as the linear response of vortex creep in those regions of the pinned superfluid in the neutron star crust through which no sudden vortex motion occurred at the time of the glitch. The long-term recovery is interpreted as the nonlinear response of vortex creep regions. In addition, there are regions of the crustal superfluid which cannot sustain a vortex density or vortex creep current, but which play a significant role in determining the angular momentum balance. The tendency of glitches to leave permanent spin-up remnants is explained as a discrete internal torque which in glitches, couples part of the crustal superfluid to the observed crust. We find that, on average, the theoretically expected interglitch intervals agree quite well with the observed intervals. The same set of short and intermediate relaxation times, with similar values of moments of inertia for the various components of the crustal superfluid, yield good fits for all postglitch data sets. Furthermore, these relaxation times and moments of inertia are compatible with previous theoretical estimates. A moment of inertia fraction of at least 0.024 is implied for the crustal superfluid. This result rules out neutron star models based on soft equations of state.en_US
dc.languageengen_US
dc.publisherInstitute of Physics Publishing Ltd. The Journal's web site is located at http://iopscience.iop.org/2041-8205en_US
dc.relation.ispartofAstrophysical Journal Lettersen_US
dc.subjectDense Matteren_US
dc.subjectPulsars: Individual (Vela)en_US
dc.subjectStars: Neutronen_US
dc.titlePostglitch relaxation of the vela pulsar after its first eight large glitches: A reevaluation with the vortex creep modelen_US
dc.typeArticleen_US
dc.identifier.emailChau, HF: hfchau@hku.hken_US
dc.identifier.emailCheng, KS: hrspksc@hkucc.hku.hken_US
dc.identifier.authorityChau, HF=rp00669en_US
dc.identifier.authorityCheng, KS=rp00675en_US
dc.description.naturelink_to_subscribed_fulltexten_US
dc.identifier.scopuseid_2-s2.0-12044253433en_US
dc.identifier.volume409en_US
dc.identifier.issue1en_US
dc.identifier.spage345en_US
dc.identifier.epage359en_US
dc.publisher.placeUnited Kingdomen_US
dc.identifier.scopusauthoridAli Alpar, M=6506406905en_US
dc.identifier.scopusauthoridChau, HF=7005742276en_US
dc.identifier.scopusauthoridCheng, KS=9745798500en_US
dc.identifier.scopusauthoridPines, D=16485047900en_US

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