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Article: Deep X-ray observations of the young high-magnetic-field radio pulsar J1119-6127 and supernova remnant G292.2-0.5
Title | Deep X-ray observations of the young high-magnetic-field radio pulsar J1119-6127 and supernova remnant G292.2-0.5 |
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Authors | |
Keywords | Ism: Individual Objects (G292.2-0.5) Ism: Supernova Remnants Pulsars: Individual (Psr J1119-6127) Stars: Neutron X-Rays: Ism |
Issue Date | 2012 |
Publisher | Institute 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? |
Abstract | High-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 Identifier | http://hdl.handle.net/10722/180507 |
ISSN | 2023 Impact Factor: 4.8 2023 SCImago Journal Rankings: 1.905 |
ISI Accession Number ID | |
References |
DC Field | Value | Language |
---|---|---|
dc.contributor.author | Ng, CY | en_US |
dc.contributor.author | Kaspi, VM | en_US |
dc.contributor.author | Ho, WCG | en_US |
dc.contributor.author | Weltevrede, P | en_US |
dc.contributor.author | Bogdanov, S | en_US |
dc.contributor.author | Shannon, R | en_US |
dc.contributor.author | Gonzalez, ME | en_US |
dc.date.accessioned | 2013-01-28T01:38:56Z | - |
dc.date.available | 2013-01-28T01:38:56Z | - |
dc.date.issued | 2012 | en_US |
dc.identifier.citation | Astrophysical Journal, 2012, v. 761 n. 1, article no. 65 | en_US |
dc.identifier.issn | 0004-637X | en_US |
dc.identifier.uri | http://hdl.handle.net/10722/180507 | - |
dc.description.abstract | High-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.language | eng | en_US |
dc.publisher | Institute of Physics Publishing, Inc. The Journal's web site is located at http://iopscience.iop.org/0004-637X/ | en_US |
dc.relation.ispartof | Astrophysical Journal | en_US |
dc.rights | The Astrophysical Journal. Copyright © Institute of Physics Publishing, Inc. | - |
dc.subject | Ism: Individual Objects (G292.2-0.5) | en_US |
dc.subject | Ism: Supernova Remnants | en_US |
dc.subject | Pulsars: Individual (Psr J1119-6127) | en_US |
dc.subject | Stars: Neutron | en_US |
dc.subject | X-Rays: Ism | en_US |
dc.title | Deep X-ray observations of the young high-magnetic-field radio pulsar J1119-6127 and supernova remnant G292.2-0.5 | en_US |
dc.type | Article | en_US |
dc.identifier.email | Ng, CY: stephen_ng@hku.hk | en_US |
dc.identifier.authority | Ng, CY=rp01706 | en_US |
dc.description.nature | postprint | en_US |
dc.identifier.doi | 10.1088/0004-637X/761/1/65 | en_US |
dc.identifier.scopus | eid_2-s2.0-84870378177 | en_US |
dc.identifier.hkuros | 216904 | - |
dc.relation.references | http://www.scopus.com/mlt/select.url?eid=2-s2.0-84870378177&selection=ref&src=s&origin=recordpage | en_US |
dc.identifier.volume | 761 | en_US |
dc.identifier.issue | 1 | en_US |
dc.identifier.isi | WOS:000311748800065 | - |
dc.publisher.place | United States | en_US |
dc.identifier.scopusauthorid | Ng, CY=24830903500 | en_US |
dc.identifier.scopusauthorid | Kaspi, VM=7006755510 | en_US |
dc.identifier.scopusauthorid | Ho, WCG=55507343600 | en_US |
dc.identifier.scopusauthorid | Weltevrede, P=10340986100 | en_US |
dc.identifier.scopusauthorid | Bogdanov, S=8837297200 | en_US |
dc.identifier.scopusauthorid | Shannon, R=44861629500 | en_US |
dc.identifier.scopusauthorid | Gonzalez, ME=15127443900 | en_US |
dc.identifier.issnl | 0004-637X | - |