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Article: The thermal response of A pulsar glitch: The nonspherically symmetric case

TitleThe thermal response of A pulsar glitch: The nonspherically symmetric case
Authors
KeywordsDense matter
Stars: evolution
Stars: interiors
Stars: neutron
X-rays: stars
Issue Date1998
PublisherInstitute of Physics Publishing Ltd. The Journal's web site is located at http://iopscience.iop.org/2041-8205
Citation
Astrophysical Journal Letters, 1998, v. 499 n. 1 PART II, p. L45-L48 How to Cite?
AbstractWe study the thermal evolution of a pulsar after a glitch in which the energy is released from a relatively compact region. A set of relativistic thermal transport and energy balance equations is used to study the thermal evolution, without making the assumption of spherical symmetry. We use an exact cooling model to solve this set of differential equations. Our results could differ significantly from those obtained under the assumption of spherical symmetry. Even for young pulsars with a hot core like the Vela pulsar, a detectable hot spot could be observed after a glitch if a large amount of energy is released in a small region close to the surface of the star. The results suggest that the intensity variation and the relative phases of hard X-ray emissions in different epochs may provide important information on the equation of state. © 1998. The American Astronomical Society. All rights reserved.
Persistent Identifierhttp://hdl.handle.net/10722/43239
ISSN
2015 Impact Factor: 5.487
2015 SCImago Journal Rankings: 3.369
ISI Accession Number ID
References

 

DC FieldValueLanguage
dc.contributor.authorCheng, KSen_HK
dc.contributor.authorLi, Yen_HK
dc.contributor.authorSuen, WMen_HK
dc.date.accessioned2007-03-23T04:41:58Z-
dc.date.available2007-03-23T04:41:58Z-
dc.date.issued1998en_HK
dc.identifier.citationAstrophysical Journal Letters, 1998, v. 499 n. 1 PART II, p. L45-L48en_HK
dc.identifier.issn2041-8205en_HK
dc.identifier.urihttp://hdl.handle.net/10722/43239-
dc.description.abstractWe study the thermal evolution of a pulsar after a glitch in which the energy is released from a relatively compact region. A set of relativistic thermal transport and energy balance equations is used to study the thermal evolution, without making the assumption of spherical symmetry. We use an exact cooling model to solve this set of differential equations. Our results could differ significantly from those obtained under the assumption of spherical symmetry. Even for young pulsars with a hot core like the Vela pulsar, a detectable hot spot could be observed after a glitch if a large amount of energy is released in a small region close to the surface of the star. The results suggest that the intensity variation and the relative phases of hard X-ray emissions in different epochs may provide important information on the equation of state. © 1998. The American Astronomical Society. All rights reserved.en_HK
dc.format.extent112849 bytes-
dc.format.extent12158 bytes-
dc.format.mimetypeapplication/pdf-
dc.format.mimetypetext/plain-
dc.languageengen_HK
dc.publisherInstitute of Physics Publishing Ltd. The Journal's web site is located at http://iopscience.iop.org/2041-8205en_HK
dc.relation.ispartofAstrophysical Journal Lettersen_HK
dc.rightsThe Astrophysical Journal. Copyright © University of Chicago Press.en_HK
dc.rightsCreative Commons: Attribution 3.0 Hong Kong License-
dc.subjectDense matteren_HK
dc.subjectStars: evolutionen_HK
dc.subjectStars: interiorsen_HK
dc.subjectStars: neutronen_HK
dc.subjectX-rays: starsen_HK
dc.titleThe thermal response of A pulsar glitch: The nonspherically symmetric caseen_HK
dc.typeArticleen_HK
dc.identifier.openurlhttp://library.hku.hk:4550/resserv?sid=HKU:IR&issn=0004-637X&volume=499&issue=pt 2&spage=L45&epage=L48&date=1998&atitle=The+Thermal+Response+of+a+Pulsar+Glitch:+The+Nonspherically+Symmetric+Caseen_HK
dc.identifier.emailCheng, KS: hrspksc@hkucc.hku.hken_HK
dc.identifier.emailLi, Y: Yongli@hkucc.hku.hken_HK
dc.identifier.authorityCheng, KS=rp00675en_HK
dc.identifier.authorityLi, Y=rp00743en_HK
dc.description.naturepublished_or_final_versionen_HK
dc.identifier.doi10.1086/311342en_HK
dc.identifier.scopuseid_2-s2.0-22044444808en_HK
dc.identifier.hkuros38908-
dc.relation.referenceshttp://www.scopus.com/mlt/select.url?eid=2-s2.0-22044444808&selection=ref&src=s&origin=recordpageen_HK
dc.identifier.volume499en_HK
dc.identifier.issue1 PART IIen_HK
dc.identifier.spageL45en_HK
dc.identifier.epageL48en_HK
dc.identifier.isiWOS:000073908200011-
dc.publisher.placeUnited Kingdomen_HK
dc.identifier.scopusauthoridCheng, KS=9745798500en_HK
dc.identifier.scopusauthoridLi, Y=15822576000en_HK
dc.identifier.scopusauthoridSuen, WM=7006977947en_HK

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