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Article: The effects of rotation on thermal X-ray afterglows resulting from pulsar glitches

TitleThe effects of rotation on thermal X-ray afterglows resulting from pulsar glitches
Authors
KeywordsDense matter
Stars: evolution
Stars: interiors
Stars: neutron
X-rays: stars
Issue Date2004
PublisherInstitute of Physics Publishing Ltd. The Journal's web site is located at http://iopscience.iop.org/2041-8205
Citation
Astrophysical Journal Letters, 2004, v. 608 n. 2 I, p. 935-944 How to Cite?
AbstractWe derive the anisotropic heat transport equation for rotating neutron stars, and we also derive the thermal equilibrium condition in a relativistic rotating axisymmetric star through a simple variational argument. With a simple model of a neutron star, we model the propagation of heat pulses resulting from transient energy releases inside the star. Such sudden energy release can occur in pulsars during glitches. Even in a slow rotation limit (Ω ≤ 1 × 103 s-1), the results with rotational effects involved could be noticeably different from those obtained with a spherically symmetric metric in terms of the timescales and magnitudes of thermal afterglow. We also study the effects of gravitational lensing and frame dragging on the X-ray light curve pulsations. Our results indicate that the effect of rotation on the light-curve modulation is small and that the spacetime-curvature effect predominates. The metric components and rotational deformation of the stellar structure are calculated using Hartle-Thorne formalism. We have applied our model to study the thermal response timescales of pulsars after glitches and find that the centrifugal force produced by rotation can substantially reduce the response time by a factor of 3 between a nonrotating star and a rotating star with Ω ∼ 900 s-1. The equation of state can also affect the duration of the response.
Persistent Identifierhttp://hdl.handle.net/10722/43448
ISSN
2015 Impact Factor: 5.487
2015 SCImago Journal Rankings: 3.369
ISI Accession Number ID
References

 

DC FieldValueLanguage
dc.contributor.authorHui, CYen_HK
dc.contributor.authorCheng, KSen_HK
dc.date.accessioned2007-03-23T04:45:53Z-
dc.date.available2007-03-23T04:45:53Z-
dc.date.issued2004en_HK
dc.identifier.citationAstrophysical Journal Letters, 2004, v. 608 n. 2 I, p. 935-944en_HK
dc.identifier.issn2041-8205en_HK
dc.identifier.urihttp://hdl.handle.net/10722/43448-
dc.description.abstractWe derive the anisotropic heat transport equation for rotating neutron stars, and we also derive the thermal equilibrium condition in a relativistic rotating axisymmetric star through a simple variational argument. With a simple model of a neutron star, we model the propagation of heat pulses resulting from transient energy releases inside the star. Such sudden energy release can occur in pulsars during glitches. Even in a slow rotation limit (Ω ≤ 1 × 103 s-1), the results with rotational effects involved could be noticeably different from those obtained with a spherically symmetric metric in terms of the timescales and magnitudes of thermal afterglow. We also study the effects of gravitational lensing and frame dragging on the X-ray light curve pulsations. Our results indicate that the effect of rotation on the light-curve modulation is small and that the spacetime-curvature effect predominates. The metric components and rotational deformation of the stellar structure are calculated using Hartle-Thorne formalism. We have applied our model to study the thermal response timescales of pulsars after glitches and find that the centrifugal force produced by rotation can substantially reduce the response time by a factor of 3 between a nonrotating star and a rotating star with Ω ∼ 900 s-1. The equation of state can also affect the duration of the response.en_HK
dc.format.extent541731 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 effects of rotation on thermal X-ray afterglows resulting from pulsar glitchesen_HK
dc.typeArticleen_HK
dc.identifier.openurlhttp://library.hku.hk:4550/resserv?sid=HKU:IR&issn=0004-637X&volume=608&issue=2 pt 1&spage=935&epage=944&date=2004&atitle=The+Effects+of+Rotation+on+Thermal+X-Ray+Afterglows+Resulting+from+Pulsar+Glitchesen_HK
dc.identifier.emailCheng, KS: hrspksc@hkucc.hku.hken_HK
dc.identifier.authorityCheng, KS=rp00675en_HK
dc.description.naturepublished_or_final_versionen_HK
dc.identifier.doi10.1086/420764en_HK
dc.identifier.scopuseid_2-s2.0-3142746200en_HK
dc.identifier.hkuros97120-
dc.relation.referenceshttp://www.scopus.com/mlt/select.url?eid=2-s2.0-3142746200&selection=ref&src=s&origin=recordpageen_HK
dc.identifier.volume608en_HK
dc.identifier.issue2 Ien_HK
dc.identifier.spage935en_HK
dc.identifier.epage944en_HK
dc.identifier.isiWOS:000222184300027-
dc.publisher.placeUnited Kingdomen_HK
dc.identifier.scopusauthoridHui, CY=12781234500en_HK
dc.identifier.scopusauthoridCheng, KS=9745798500en_HK

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