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Article: The pulsar wind nebula torus of PSR J0538+2817 and the origin of pulsar velocities

TitleThe pulsar wind nebula torus of PSR J0538+2817 and the origin of pulsar velocities
Authors
KeywordsPulsars: Individual (Psr J0538+2817)
Stars: Neutron
Stars: Rotation
Issue Date2003
PublisherInstitute of Physics Publishing Ltd. The Journal's web site is located at http://iopscience.iop.org/2041-8205
Citation
Astrophysical Journal Letters, 2003, v. 585 n. 1 II, p. L41-L44 How to Cite?
AbstractWe find evidence for a faint wind nebula surrounding PSR J0538+2817 in Chandra X-Ray Observatory ACIS imaging. This object is particularly interesting, as the pulsar spin-down age is largest for any such X-ray pulsar wind nebula (PWN). If interpreted as an equatorial torus, the PWN supports the claimed association with the S147 supernova remnant and implies good alignment between the pulsar spin and space velocity. Comparison of the supernova remnant age, X-ray cooling age, and characteristic age suggests a birth spin period of ⊇ 130 ms. In turn, if we accept as causal the alignment of the linear and angular momenta, this places strong constraints on the origin of the "kick" at the neutron star birth.
Persistent Identifierhttp://hdl.handle.net/10722/180479
ISSN
2015 Impact Factor: 5.487
2015 SCImago Journal Rankings: 3.369
ISI Accession Number ID
References

 

DC FieldValueLanguage
dc.contributor.authorRomani, RWen_US
dc.contributor.authorNg, CYen_US
dc.date.accessioned2013-01-28T01:38:43Z-
dc.date.available2013-01-28T01:38:43Z-
dc.date.issued2003en_US
dc.identifier.citationAstrophysical Journal Letters, 2003, v. 585 n. 1 II, p. L41-L44en_US
dc.identifier.issn2041-8205en_US
dc.identifier.urihttp://hdl.handle.net/10722/180479-
dc.description.abstractWe find evidence for a faint wind nebula surrounding PSR J0538+2817 in Chandra X-Ray Observatory ACIS imaging. This object is particularly interesting, as the pulsar spin-down age is largest for any such X-ray pulsar wind nebula (PWN). If interpreted as an equatorial torus, the PWN supports the claimed association with the S147 supernova remnant and implies good alignment between the pulsar spin and space velocity. Comparison of the supernova remnant age, X-ray cooling age, and characteristic age suggests a birth spin period of ⊇ 130 ms. In turn, if we accept as causal the alignment of the linear and angular momenta, this places strong constraints on the origin of the "kick" at the neutron star birth.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: Individual (Psr J0538+2817)en_US
dc.subjectStars: Neutronen_US
dc.subjectStars: Rotationen_US
dc.titleThe pulsar wind nebula torus of PSR J0538+2817 and the origin of pulsar velocitiesen_US
dc.typeArticleen_US
dc.identifier.emailNg, CY: stephen_ng@hku.hken_US
dc.identifier.authorityNg, CY=rp01706en_US
dc.description.naturelink_to_OA_fulltexten_US
dc.identifier.doi10.1086/374259en_US
dc.identifier.scopuseid_2-s2.0-0041878943en_US
dc.relation.referenceshttp://www.scopus.com/mlt/select.url?eid=2-s2.0-0041878943&selection=ref&src=s&origin=recordpageen_US
dc.identifier.volume585en_US
dc.identifier.issue1 IIen_US
dc.identifier.spageL41en_US
dc.identifier.epageL44en_US
dc.identifier.isiWOS:000181046600011-
dc.publisher.placeUnited Kingdomen_US
dc.identifier.scopusauthoridRomani, RW=35248859100en_US
dc.identifier.scopusauthoridNg, CY=24830903500en_US

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