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Article: Postglitch relaxation of the Crab pulsar: Evidence for crust cracking

TitlePostglitch relaxation of the Crab pulsar: Evidence for crust cracking
Authors
KeywordsDense Matter
Pulsars: Individual (Crab Pulsar)
Stars: Neutron
Issue Date1994
PublisherInstitute of Physics Publishing Ltd. The Journal's web site is located at http://iopscience.iop.org/2041-8205
Citation
Astrophysical Journal Letters, 1994, v. 427 n. 1 PART 2, p. L29-L31 How to Cite?
AbstractThe pattern of glitches and postglitch behavior observed for the Crab pulsar (Boynton et al. 1972; Demiański & Prószyński 1983; Lyne & Pritchard 1987; Lyne, Graham-Smith, & Pritchard 1992) is strikingly different from that observed for the Vela pulsar (Alpar et al. 1993). A key question is whether the differences can be understood on evolutionary grounds. An analysis of the Crab pulsar suggests that this is indeed the case. Thus, we propose that the comparatively modest (ΔΩ/Ω ∼ 10 -8) and somewhat infrequent (∼6 yr interglitch intervals) Crab pulsar glitches are caused by starquakes induced by pulsar spin-down (Ruderman 1976; Baym & Pines 1971); we attribute its anomalous postglitch behavior (an occasional extended spin-up and a long-term response opposite in sign to that seen in the Vela pulsar (Lyne et al. 1992) to vortices transported inward during a quake, while the observed unexpected persistent change in angular acceleration, Ω̇ e, following a glitch represents the creation of a new vortex depletion region, as suggested by Alpar & Pines (1993).
Persistent Identifierhttp://hdl.handle.net/10722/174907
ISSN
2015 Impact Factor: 5.487
2015 SCImago Journal Rankings: 3.369

 

DC FieldValueLanguage
dc.contributor.authorAlpar, MAen_US
dc.contributor.authorChau, HFen_US
dc.contributor.authorCheng, KSen_US
dc.contributor.authorPines, Den_US
dc.date.accessioned2012-11-26T08:48:04Z-
dc.date.available2012-11-26T08:48:04Z-
dc.date.issued1994en_US
dc.identifier.citationAstrophysical Journal Letters, 1994, v. 427 n. 1 PART 2, p. L29-L31en_US
dc.identifier.issn2041-8205en_US
dc.identifier.urihttp://hdl.handle.net/10722/174907-
dc.description.abstractThe pattern of glitches and postglitch behavior observed for the Crab pulsar (Boynton et al. 1972; Demiański & Prószyński 1983; Lyne & Pritchard 1987; Lyne, Graham-Smith, & Pritchard 1992) is strikingly different from that observed for the Vela pulsar (Alpar et al. 1993). A key question is whether the differences can be understood on evolutionary grounds. An analysis of the Crab pulsar suggests that this is indeed the case. Thus, we propose that the comparatively modest (ΔΩ/Ω ∼ 10 -8) and somewhat infrequent (∼6 yr interglitch intervals) Crab pulsar glitches are caused by starquakes induced by pulsar spin-down (Ruderman 1976; Baym & Pines 1971); we attribute its anomalous postglitch behavior (an occasional extended spin-up and a long-term response opposite in sign to that seen in the Vela pulsar (Lyne et al. 1992) to vortices transported inward during a quake, while the observed unexpected persistent change in angular acceleration, Ω̇ e, following a glitch represents the creation of a new vortex depletion region, as suggested by Alpar & Pines (1993).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 (Crab Pulsar)en_US
dc.subjectStars: Neutronen_US
dc.titlePostglitch relaxation of the Crab pulsar: Evidence for crust crackingen_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-s2.0-12044250944en_US
dc.identifier.volume427en_US
dc.identifier.issue1 PART 2en_US
dc.identifier.spageL29en_US
dc.identifier.epageL31en_US
dc.publisher.placeUnited Kingdomen_US
dc.identifier.scopusauthoridAlpar, MA=6701508412en_US
dc.identifier.scopusauthoridChau, HF=7005742276en_US
dc.identifier.scopusauthoridCheng, KS=9745798500en_US
dc.identifier.scopusauthoridPines, D=16485047900en_US

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