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Article: Effects of evolving rotating equilibrium configurations on the cooling and spin-down of pulsars

TitleEffects of evolving rotating equilibrium configurations on the cooling and spin-down of pulsars
Authors
KeywordsPulsars: General
Radiation Mechanisms: Miscellaneous
Stars: Rotation
Issue Date1992
PublisherInstitute of Physics Publishing Ltd. The Journal's web site is located at http://iopscience.iop.org/2041-8205
Citation
Astrophysical Journal Letters, 1992, v. 396 n. 1, p. 135-146 How to Cite?
AbstractWe model a pulsar by a uniform density rotating spheroid covered by a solid crust. During the spin-down (up) epoch, pulsars can adjust their shapes to their equilibrium configurations, which depend on the stellar rotation velocity Ω, due to plastic flow and continuous crust breaking resulting from various mechanisms even though the crust is supposedly rigid. We show that this results in a coupling among the stellar temperature (T). the rotation velocity (Ω) and the eccentricity (e). and cooling and spin-down therefore mutually affect each other. Theoretically, crust cracking could be the dominant heating mechanism for pulsars instead of the vortex creeping mechanism if the crust is an ideal Coulomb lattice. But the present observed X-ray data can only provide constraints on the parameters of these two heating mechanisms and cannot determine which is the dominant one. For weak field millisecond pulsars, either one can lead to heating balancing the blackbody cooling, thus making these pulsars persistent soft X-ray emitters. Other implications and observational consequences of these heating mechanisms are discussed in the text.
Persistent Identifierhttp://hdl.handle.net/10722/174618
ISSN
2015 Impact Factor: 5.487
2015 SCImago Journal Rankings: 3.369

 

DC FieldValueLanguage
dc.contributor.authorCheng, KSen_US
dc.contributor.authorChau, WYen_US
dc.contributor.authorZhang, JLen_US
dc.contributor.authorChau, HFen_US
dc.date.accessioned2012-11-26T08:46:33Z-
dc.date.available2012-11-26T08:46:33Z-
dc.date.issued1992en_US
dc.identifier.citationAstrophysical Journal Letters, 1992, v. 396 n. 1, p. 135-146en_US
dc.identifier.issn2041-8205en_US
dc.identifier.urihttp://hdl.handle.net/10722/174618-
dc.description.abstractWe model a pulsar by a uniform density rotating spheroid covered by a solid crust. During the spin-down (up) epoch, pulsars can adjust their shapes to their equilibrium configurations, which depend on the stellar rotation velocity Ω, due to plastic flow and continuous crust breaking resulting from various mechanisms even though the crust is supposedly rigid. We show that this results in a coupling among the stellar temperature (T). the rotation velocity (Ω) and the eccentricity (e). and cooling and spin-down therefore mutually affect each other. Theoretically, crust cracking could be the dominant heating mechanism for pulsars instead of the vortex creeping mechanism if the crust is an ideal Coulomb lattice. But the present observed X-ray data can only provide constraints on the parameters of these two heating mechanisms and cannot determine which is the dominant one. For weak field millisecond pulsars, either one can lead to heating balancing the blackbody cooling, thus making these pulsars persistent soft X-ray emitters. Other implications and observational consequences of these heating mechanisms are discussed in the text.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.subjectPulsars: Generalen_US
dc.subjectRadiation Mechanisms: Miscellaneousen_US
dc.subjectStars: Rotationen_US
dc.titleEffects of evolving rotating equilibrium configurations on the cooling and spin-down of pulsarsen_US
dc.typeArticleen_US
dc.identifier.emailCheng, KS: hrspksc@hkucc.hku.hken_US
dc.identifier.emailChau, HF: hfchau@hku.hken_US
dc.identifier.authorityCheng, KS=rp00675en_US
dc.identifier.authorityChau, HF=rp00669en_US
dc.description.naturelink_to_subscribed_fulltexten_US
dc.identifier.scopuseid_2-s2.0-0000650879en_US
dc.identifier.volume396en_US
dc.identifier.issue1en_US
dc.identifier.spage135en_US
dc.identifier.epage146en_US
dc.publisher.placeUnited Kingdomen_US
dc.identifier.scopusauthoridCheng, KS=9745798500en_US
dc.identifier.scopusauthoridChau, WY=7006157958en_US
dc.identifier.scopusauthoridZhang, JL=14039783200en_US
dc.identifier.scopusauthoridChau, HF=7005742276en_US

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