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Article: The X-ray properties of the energetic pulsar PSR J1838-0655

TitleThe X-ray properties of the energetic pulsar PSR J1838-0655
Authors
KeywordsGamma-rays: Observations
Line: Identification
Pulsars: General
Radiation mechanisms: general
X-rays: General
Issue Date2009
PublisherBlackwell Publishing Ltd. The Journal's web site is located at http://www.blackwellpublishing.com/journals/MNR
Citation
Monthly Notices Of The Royal Astronomical Society, 2009, v. 400 n. 1, p. 168-175 How to Cite?
AbstractWe present and interpret several new X-ray features of the X-ray pulsar PSR J1838-0655. The X-ray data are obtained from the archival data of Chandra, RXTE and Suzaku. We combine all these X-ray data and fit the spectra with different models. We find that the joint spectra are difficult to fit with a single power law; a broken power-law model with a break at around 6.5 keV can improve the fit significantly. The photon index changes from Γ = 1.0 (below 6.5 keV) to 1.5 (above 6.5 keV); this indicates a softer spectral behaviour at hard X-rays. The X-ray flux at 2-20 keV is found to be 1.6 × 10-11 erg cm-2 s-1. The conversion efficiency from the spin-down luminosity is ∼0.9 per cent at 0.8-10 keV, which is much higher than that (∼10-3 to 10-4 per cent) of the pulsars that show similar timing properties. We discuss non-thermal radiation mechanisms for the observed high X-ray conversion efficiency and find that emission from the magnetosphere of a greatly inclined rotator is the most favourable interpretation for the conversion rate and the pulse profiles at X-ray bands. A line feature close to 6.65 keV is also detected in the spectra of Suzaku/X-ray imaging spectrometer; it might be the Kα emission of highly ionized Fe surrounding the pulsar. © 2009 RAS.
Persistent Identifierhttp://hdl.handle.net/10722/134623
ISSN
2015 Impact Factor: 4.952
2015 SCImago Journal Rankings: 2.806
ISI Accession Number ID
Funding AgencyGrant Number
National Science CouncilNSC 98-2811-M-008-044
NSC 96-2112-M-008-017-MY3
NSC 95-2923-M-008-001-MY3
NSC 96-2752-M-007-007-PAE
Theoretical Institute for Advanced Research in Astrophysics (TIARA)
Funding Information:

The authors thank an anonymous referee for his/her helpful comments. We also thank Dr. Albert Kong for the careful review of the manuscript and thank Drs. Hsiang-Kuang Chang, Kwong-Sang Cheng and Ronald Taam for fruitful discussion. This research has made use of the data obtained through the High Energy Astrophysics Science Archive Research Center Online Service, provided by the NASA/Goddard Space Flight Center. This work was partially supported by the National Science Council through grants NSC 98-2811-M-008-044. CYH acknowledges support from the National Science Council through grants NSC 96-2112-M-008-017-MY3 and NSC 95-2923-M-008-001-MY3. JT was supported by the Theoretical Institute for Advanced Research in Astrophysics (TIARA), operated under Academia Sinica and the National Science Council Excellence Projects program in Taiwan through grant NSC 96-2752-M-007-007-PAE.

References

 

DC FieldValueLanguage
dc.contributor.authorChunChe Lin, Len_HK
dc.contributor.authorTakata, Jen_HK
dc.contributor.authorHwang, CYen_HK
dc.contributor.authorLiang, JSen_HK
dc.date.accessioned2011-06-29T06:39:18Z-
dc.date.available2011-06-29T06:39:18Z-
dc.date.issued2009en_HK
dc.identifier.citationMonthly Notices Of The Royal Astronomical Society, 2009, v. 400 n. 1, p. 168-175en_HK
dc.identifier.issn0035-8711en_HK
dc.identifier.urihttp://hdl.handle.net/10722/134623-
dc.description.abstractWe present and interpret several new X-ray features of the X-ray pulsar PSR J1838-0655. The X-ray data are obtained from the archival data of Chandra, RXTE and Suzaku. We combine all these X-ray data and fit the spectra with different models. We find that the joint spectra are difficult to fit with a single power law; a broken power-law model with a break at around 6.5 keV can improve the fit significantly. The photon index changes from Γ = 1.0 (below 6.5 keV) to 1.5 (above 6.5 keV); this indicates a softer spectral behaviour at hard X-rays. The X-ray flux at 2-20 keV is found to be 1.6 × 10-11 erg cm-2 s-1. The conversion efficiency from the spin-down luminosity is ∼0.9 per cent at 0.8-10 keV, which is much higher than that (∼10-3 to 10-4 per cent) of the pulsars that show similar timing properties. We discuss non-thermal radiation mechanisms for the observed high X-ray conversion efficiency and find that emission from the magnetosphere of a greatly inclined rotator is the most favourable interpretation for the conversion rate and the pulse profiles at X-ray bands. A line feature close to 6.65 keV is also detected in the spectra of Suzaku/X-ray imaging spectrometer; it might be the Kα emission of highly ionized Fe surrounding the pulsar. © 2009 RAS.en_HK
dc.languageeng-
dc.publisherBlackwell Publishing Ltd. The Journal's web site is located at http://www.blackwellpublishing.com/journals/MNRen_HK
dc.relation.ispartofMonthly Notices of the Royal Astronomical Societyen_HK
dc.rightsThe definitive version is available at www.blackwell-synergy.com-
dc.subjectGamma-rays: Observationsen_HK
dc.subjectLine: Identificationen_HK
dc.subjectPulsars: Generalen_HK
dc.subjectRadiation mechanisms: generalen_HK
dc.subjectX-rays: Generalen_HK
dc.titleThe X-ray properties of the energetic pulsar PSR J1838-0655en_HK
dc.typeArticleen_HK
dc.identifier.openurlhttp://library.hku.hk:4550/resserv?sid=HKU:IR&issn=0035-8711&volume=400&issue=1&spage=168&epage=175&date=2009&atitle=The+X-ray+properties+of+the+energetic+pulsar+PSR+J1838-0655-
dc.identifier.emailTakata, J: takata@hku.hken_HK
dc.identifier.authorityTakata, J=rp00786en_HK
dc.description.naturelink_to_subscribed_fulltext-
dc.identifier.doi10.1111/j.1365-2966.2009.15468.xen_HK
dc.identifier.scopuseid_2-s2.0-70449572159en_HK
dc.identifier.hkuros170775-
dc.relation.referenceshttp://www.scopus.com/mlt/select.url?eid=2-s2.0-70449572159&selection=ref&src=s&origin=recordpageen_HK
dc.identifier.volume400en_HK
dc.identifier.issue1en_HK
dc.identifier.spage168en_HK
dc.identifier.epage175en_HK
dc.identifier.isiWOS:000271708900036-
dc.publisher.placeUnited Kingdomen_HK
dc.identifier.scopusauthoridChunChe Lin, L=35172698400en_HK
dc.identifier.scopusauthoridTakata, J=22735157300en_HK
dc.identifier.scopusauthoridHwang, CY=7403387605en_HK
dc.identifier.scopusauthoridLiang, JS=14063635300en_HK

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