File Download
  Links for fulltext
     (May Require Subscription)
Supplementary

Article: Deep X-ray observations of the young high-magnetic-field radio pulsar J1119-6127 and supernova remnant G292.2-0.5

TitleDeep X-ray observations of the young high-magnetic-field radio pulsar J1119-6127 and supernova remnant G292.2-0.5
Authors
KeywordsIsm: Individual Objects (G292.2-0.5)
Ism: Supernova Remnants
Pulsars: Individual (Psr J1119-6127)
Stars: Neutron
X-Rays: Ism
Issue Date2012
PublisherInstitute of Physics Publishing, Inc. The Journal's web site is located at http://iopscience.iop.org/0004-637X/
Citation
Astrophysical Journal, 2012, v. 761 n. 1, article no. 65 How to Cite?
AbstractHigh-magnetic-field radio pulsars are important transition objects for understanding the connection between magnetars and conventional radio pulsars. We present a detailed study of the young radio pulsar J1119-6127, which has a characteristic age of 1900 yr and a spin-down-inferred magnetic field of 4.1 × 10 13 G, and its associated supernova remnant G292.2-0.5, using deep XMM-Newton and Chandra X-ray Observatory exposures of over 120 ks from each telescope. The pulsar emission shows strong modulation below 2.5 keV with a single-peaked profile and a large pulsed fraction of 0.48 ± 0.12. Employing a magnetic, partially ionized hydrogen atmosphere model, we find that the observed pulse profile can be produced by a single hot spot of temperature 0.13 keV covering about one-third of the stellar surface, and we place an upper limit of 0.08 keV for an antipodal hot spot with the same area. The non-uniform surface temperature distribution could be the result of anisotropic heat conduction under a strong magnetic field, and a single-peaked profile seems common among high-B radio pulsars. For the associated remnant G292.2-0.5, its large diameter could be attributed to fast expansion in a low-density wind cavity, likely formed by a Wolf-Rayet progenitor, similar to two other high-B radio pulsars. © 2012. The American Astronomical Society. All rights reserved..
Persistent Identifierhttp://hdl.handle.net/10722/180507
ISSN
2015 Impact Factor: 5.909
2015 SCImago Journal Rankings: 3.266
ISI Accession Number ID
References

 

DC FieldValueLanguage
dc.contributor.authorNg, CYen_US
dc.contributor.authorKaspi, VMen_US
dc.contributor.authorHo, WCGen_US
dc.contributor.authorWeltevrede, Pen_US
dc.contributor.authorBogdanov, Sen_US
dc.contributor.authorShannon, Ren_US
dc.contributor.authorGonzalez, MEen_US
dc.date.accessioned2013-01-28T01:38:56Z-
dc.date.available2013-01-28T01:38:56Z-
dc.date.issued2012en_US
dc.identifier.citationAstrophysical Journal, 2012, v. 761 n. 1, article no. 65en_US
dc.identifier.issn0004-637Xen_US
dc.identifier.urihttp://hdl.handle.net/10722/180507-
dc.description.abstractHigh-magnetic-field radio pulsars are important transition objects for understanding the connection between magnetars and conventional radio pulsars. We present a detailed study of the young radio pulsar J1119-6127, which has a characteristic age of 1900 yr and a spin-down-inferred magnetic field of 4.1 × 10 13 G, and its associated supernova remnant G292.2-0.5, using deep XMM-Newton and Chandra X-ray Observatory exposures of over 120 ks from each telescope. The pulsar emission shows strong modulation below 2.5 keV with a single-peaked profile and a large pulsed fraction of 0.48 ± 0.12. Employing a magnetic, partially ionized hydrogen atmosphere model, we find that the observed pulse profile can be produced by a single hot spot of temperature 0.13 keV covering about one-third of the stellar surface, and we place an upper limit of 0.08 keV for an antipodal hot spot with the same area. The non-uniform surface temperature distribution could be the result of anisotropic heat conduction under a strong magnetic field, and a single-peaked profile seems common among high-B radio pulsars. For the associated remnant G292.2-0.5, its large diameter could be attributed to fast expansion in a low-density wind cavity, likely formed by a Wolf-Rayet progenitor, similar to two other high-B radio pulsars. © 2012. The American Astronomical Society. All rights reserved..en_US
dc.languageengen_US
dc.publisherInstitute of Physics Publishing, Inc. The Journal's web site is located at http://iopscience.iop.org/0004-637X/en_US
dc.relation.ispartofAstrophysical Journalen_US
dc.rightsThe Astrophysical Journal. Copyright © Institute of Physics Publishing, Inc.-
dc.rightsCreative Commons: Attribution 3.0 Hong Kong License-
dc.subjectIsm: Individual Objects (G292.2-0.5)en_US
dc.subjectIsm: Supernova Remnantsen_US
dc.subjectPulsars: Individual (Psr J1119-6127)en_US
dc.subjectStars: Neutronen_US
dc.subjectX-Rays: Ismen_US
dc.titleDeep X-ray observations of the young high-magnetic-field radio pulsar J1119-6127 and supernova remnant G292.2-0.5en_US
dc.typeArticleen_US
dc.identifier.emailNg, CY: stephen_ng@hku.hken_US
dc.identifier.authorityNg, CY=rp01706en_US
dc.description.naturepostprinten_US
dc.identifier.doi10.1088/0004-637X/761/1/65en_US
dc.identifier.scopuseid_2-s2.0-84870378177en_US
dc.identifier.hkuros216904-
dc.relation.referenceshttp://www.scopus.com/mlt/select.url?eid=2-s2.0-84870378177&selection=ref&src=s&origin=recordpageen_US
dc.identifier.volume761en_US
dc.identifier.issue1en_US
dc.identifier.isiWOS:000311748800065-
dc.publisher.placeUnited Statesen_US
dc.identifier.scopusauthoridNg, CY=24830903500en_US
dc.identifier.scopusauthoridKaspi, VM=7006755510en_US
dc.identifier.scopusauthoridHo, WCG=55507343600en_US
dc.identifier.scopusauthoridWeltevrede, P=10340986100en_US
dc.identifier.scopusauthoridBogdanov, S=8837297200en_US
dc.identifier.scopusauthoridShannon, R=44861629500en_US
dc.identifier.scopusauthoridGonzalez, ME=15127443900en_US

Export via OAI-PMH Interface in XML Formats


OR


Export to Other Non-XML Formats