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Article: A multiwavelength study of the pulsar PSR B1929+10 and its x-ray trail

TitleA multiwavelength study of the pulsar PSR B1929+10 and its x-ray trail
Authors
KeywordsPulsars: General
Pulsars: Individual (Psr B1929+10)
Stars: Neutron
X-Rays: Stars
Issue Date2006
PublisherInstitute of Physics Publishing Ltd. The Journal's web site is located at http://iopscience.iop.org/2041-8205
Citation
Astrophysical Journal Letters, 2006, v. 645 n. 2 I, p. 1421-1435 How to Cite?
AbstractWe report on the emission properties of PSR B1929+10 and its putative trail from a multiwavelength study performed using optical, X-ray, and radio data. XMM-Newton observations confirm the existence of the diffuse emission with a trail morphology lying in a direction opposite to the transverse motion of the pulsar. The trail spectrum is nonthermal and produced by electron-synchrotron emission in the shock between the pulsar wind and the surrounding medium. Radio data from the Effelsberg 11 cm radio continuum survey show an elongated feature that roughly coincides with the X-ray trail. Three not fully resolved radio sources seen in the NVSS survey data at 1.4 GHz match with part of the elongated radio feature seen at 11 cm. The emission properties observed from PSR B1929+10 are in excellent agreement with a nonthermal, and thus magnetospheric- radiation-dominated, emission scenario. The pulsar's X-ray spectrum is best described by a single power-law model with a photon index of 2.72 -0.09 +0.12. A flux contribution from the thermal emission of heated polar caps of at most ∼7% is inferred from a best-fitting composite Planckian and power-law spectral model. A pure thermal emission spectrum consisting of two Planckian spectra is regarded as unlikely. A broken power-law spectral model with E break = 0.83 -0.03 +0.05 keV and the photon indexes α 1 = 1.12 -0.03 +0.02 and α 2 = 2.48 -0.07 +0.08 can describe the optical and X-ray data entirely in terms of a nonthermal magnetospheric origin. The X-ray pulse profile observed in the 0.2-10 keV band is found to be markedly different from the broad sinusoidal pulse profile seen in the low statistic Röntgensatellit (ROSAT) data. Fitting Gaussians to the X-ray light curve indicates the possible existence of three pulse components. A small narrow pulse, characterized by energies greater than 1 keV, is found to lead the radio main pulse by ∼20°. The fraction of pulsed photons in the 0.2-10 keV band is 32% ± 4%. For the subbands 0.2-1.0 and 1.0-2.1 keV the pulsed fraction is 24% ± 5% and 44% ± 6%, respectively, indicating a mild energy dependence at a ∼2 σ level. Simulations in the framework of an outer gap emission model are able to reproduce the observed X-ray pulse profile and its phase shift relative to the radio pulse. © 2006. The American Astronomical Society. All rights reserved.
Persistent Identifierhttp://hdl.handle.net/10722/175025
ISSN
2015 Impact Factor: 5.487
2015 SCImago Journal Rankings: 3.369
ISI Accession Number ID
References

 

DC FieldValueLanguage
dc.contributor.authorBecker, Wen_US
dc.contributor.authorKramer, Men_US
dc.contributor.authorJessner, Aen_US
dc.contributor.authorTaam, REen_US
dc.contributor.authorJia, JJen_US
dc.contributor.authorCheng, KSen_US
dc.contributor.authorMignani, Ren_US
dc.contributor.authorPellizzoni, Aen_US
dc.contributor.authorDe Luca, Aen_US
dc.contributor.authorSłowikowska, Aen_US
dc.contributor.authorCaraveo, PAen_US
dc.date.accessioned2012-11-26T08:48:50Z-
dc.date.available2012-11-26T08:48:50Z-
dc.date.issued2006en_US
dc.identifier.citationAstrophysical Journal Letters, 2006, v. 645 n. 2 I, p. 1421-1435en_US
dc.identifier.issn2041-8205en_US
dc.identifier.urihttp://hdl.handle.net/10722/175025-
dc.description.abstractWe report on the emission properties of PSR B1929+10 and its putative trail from a multiwavelength study performed using optical, X-ray, and radio data. XMM-Newton observations confirm the existence of the diffuse emission with a trail morphology lying in a direction opposite to the transverse motion of the pulsar. The trail spectrum is nonthermal and produced by electron-synchrotron emission in the shock between the pulsar wind and the surrounding medium. Radio data from the Effelsberg 11 cm radio continuum survey show an elongated feature that roughly coincides with the X-ray trail. Three not fully resolved radio sources seen in the NVSS survey data at 1.4 GHz match with part of the elongated radio feature seen at 11 cm. The emission properties observed from PSR B1929+10 are in excellent agreement with a nonthermal, and thus magnetospheric- radiation-dominated, emission scenario. The pulsar's X-ray spectrum is best described by a single power-law model with a photon index of 2.72 -0.09 +0.12. A flux contribution from the thermal emission of heated polar caps of at most ∼7% is inferred from a best-fitting composite Planckian and power-law spectral model. A pure thermal emission spectrum consisting of two Planckian spectra is regarded as unlikely. A broken power-law spectral model with E break = 0.83 -0.03 +0.05 keV and the photon indexes α 1 = 1.12 -0.03 +0.02 and α 2 = 2.48 -0.07 +0.08 can describe the optical and X-ray data entirely in terms of a nonthermal magnetospheric origin. The X-ray pulse profile observed in the 0.2-10 keV band is found to be markedly different from the broad sinusoidal pulse profile seen in the low statistic Röntgensatellit (ROSAT) data. Fitting Gaussians to the X-ray light curve indicates the possible existence of three pulse components. A small narrow pulse, characterized by energies greater than 1 keV, is found to lead the radio main pulse by ∼20°. The fraction of pulsed photons in the 0.2-10 keV band is 32% ± 4%. For the subbands 0.2-1.0 and 1.0-2.1 keV the pulsed fraction is 24% ± 5% and 44% ± 6%, respectively, indicating a mild energy dependence at a ∼2 σ level. Simulations in the framework of an outer gap emission model are able to reproduce the observed X-ray pulse profile and its phase shift relative to the radio pulse. © 2006. The American Astronomical Society. All rights reserved.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: Generalen_US
dc.subjectPulsars: Individual (Psr B1929+10)en_US
dc.subjectStars: Neutronen_US
dc.subjectX-Rays: Starsen_US
dc.titleA multiwavelength study of the pulsar PSR B1929+10 and its x-ray trailen_US
dc.typeArticleen_US
dc.identifier.emailCheng, KS: hrspksc@hkucc.hku.hken_US
dc.identifier.authorityCheng, KS=rp00675en_US
dc.description.naturelink_to_subscribed_fulltexten_US
dc.identifier.doi10.1086/504458en_US
dc.identifier.scopuseid_2-s2.0-33746915685en_US
dc.relation.referenceshttp://www.scopus.com/mlt/select.url?eid=2-s2.0-33746915685&selection=ref&src=s&origin=recordpageen_US
dc.identifier.volume645en_US
dc.identifier.issue2 Ien_US
dc.identifier.spage1421en_US
dc.identifier.epage1435en_US
dc.identifier.isiWOS:000239053900056-
dc.publisher.placeUnited Kingdomen_US
dc.identifier.scopusauthoridBecker, W=7402414276en_US
dc.identifier.scopusauthoridKramer, M=23968081200en_US
dc.identifier.scopusauthoridJessner, A=6603889836en_US
dc.identifier.scopusauthoridTaam, RE=7003756329en_US
dc.identifier.scopusauthoridJia, JJ=36865537900en_US
dc.identifier.scopusauthoridCheng, KS=9745798500en_US
dc.identifier.scopusauthoridMignani, R=35517333300en_US
dc.identifier.scopusauthoridPellizzoni, A=6603455643en_US
dc.identifier.scopusauthoridDe Luca, A=13609305500en_US
dc.identifier.scopusauthoridSŁowikowska, A=9432975600en_US
dc.identifier.scopusauthoridCaraveo, PA=14006843000en_US

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