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Article: X-Ray and Radio Variabilities of PSR J2032+4127 near Periastron

TitleX-Ray and Radio Variabilities of PSR J2032+4127 near Periastron
Authors
Keywordspulsars: individual (PSR J2032+4127)
stars: individual (MT91 213)
stars: neutron
X-rays: binaries
X-rays: individual (PSR J2032+4127)
Issue Date2019
PublisherAmerican Astronomical Society, co-published with Institute of Physics Publishing, Inc. The Journal's web site is located at http://iopscience.iop.org/0004-637X/
Citation
The Astrophysical Journal, 2019, v. 880 n. 2, p. article no. 147 How to Cite?
AbstractWe present X-ray and radio monitoring observations of the gamma-ray binary PSR J2032+4127/MT91 213 during its periastron passage in late 2017. Dedicated Chandra, XMM-Newton, NuSTAR X-ray observations, and Very Large Array radio observations of this long orbit (50 yr), 143 ms pulsar/Be star system clearly revealed flux and spectral variability during the passage. The X-ray spectrum hardened near periastron, with a significant decrease in the power-law (PL) photon index from Γ ≈ 2 to 1.2 and evidence of an increased absorption column density. We identified a possible spectral break at a few keV in the spectrum that suggests synchrotron cooling. A coincident radio and X-ray flare occurred one week after periastron, which is possibly the result of the pulsar wind interacting with the Be stellar disk and generating synchrotron radiation. However, a multiwavelength comparison indicates that the X-ray and radio spectra cannot be simply connected by a single PL component. Hence, the emission in these two energy bands must originate from different particle populations.
Persistent Identifierhttp://hdl.handle.net/10722/273999
ISSN
2023 Impact Factor: 4.8
2023 SCImago Journal Rankings: 1.905
ISI Accession Number ID

 

DC FieldValueLanguage
dc.contributor.authorNg, CY-
dc.contributor.authorHo, WCG-
dc.contributor.authorGotthelf, EV-
dc.contributor.authorHalpern, JP-
dc.contributor.authorCoe, MJ-
dc.contributor.authorStappers, BW-
dc.contributor.authorLyne, AG-
dc.contributor.authorWood, KS-
dc.contributor.authorKerr, M-
dc.date.accessioned2019-08-18T14:53:02Z-
dc.date.available2019-08-18T14:53:02Z-
dc.date.issued2019-
dc.identifier.citationThe Astrophysical Journal, 2019, v. 880 n. 2, p. article no. 147-
dc.identifier.issn0004-637X-
dc.identifier.urihttp://hdl.handle.net/10722/273999-
dc.description.abstractWe present X-ray and radio monitoring observations of the gamma-ray binary PSR J2032+4127/MT91 213 during its periastron passage in late 2017. Dedicated Chandra, XMM-Newton, NuSTAR X-ray observations, and Very Large Array radio observations of this long orbit (50 yr), 143 ms pulsar/Be star system clearly revealed flux and spectral variability during the passage. The X-ray spectrum hardened near periastron, with a significant decrease in the power-law (PL) photon index from Γ ≈ 2 to 1.2 and evidence of an increased absorption column density. We identified a possible spectral break at a few keV in the spectrum that suggests synchrotron cooling. A coincident radio and X-ray flare occurred one week after periastron, which is possibly the result of the pulsar wind interacting with the Be stellar disk and generating synchrotron radiation. However, a multiwavelength comparison indicates that the X-ray and radio spectra cannot be simply connected by a single PL component. Hence, the emission in these two energy bands must originate from different particle populations.-
dc.languageeng-
dc.publisherAmerican Astronomical Society, co-published with Institute of Physics Publishing, Inc. The Journal's web site is located at http://iopscience.iop.org/0004-637X/-
dc.relation.ispartofThe Astrophysical Journal-
dc.rightsThe Astrophysical Journal. Copyright © American Astronomical Society, co-published with Institute of Physics Publishing, Inc.-
dc.subjectpulsars: individual (PSR J2032+4127)-
dc.subjectstars: individual (MT91 213)-
dc.subjectstars: neutron-
dc.subjectX-rays: binaries-
dc.subjectX-rays: individual (PSR J2032+4127)-
dc.titleX-Ray and Radio Variabilities of PSR J2032+4127 near Periastron-
dc.typeArticle-
dc.identifier.emailNg, CY: ncy@astro.physics.hku.hk-
dc.identifier.authorityNg, CY=rp01706-
dc.description.naturepublished_or_final_version-
dc.identifier.doi10.3847/1538-4357/ab2adb-
dc.identifier.scopuseid_2-s2.0-85071985284-
dc.identifier.hkuros301647-
dc.identifier.volume880-
dc.identifier.issue2-
dc.identifier.spagearticle no. 147-
dc.identifier.epagearticle no. 147-
dc.identifier.isiWOS:000478952800010-
dc.publisher.placeUnited States-
dc.identifier.issnl0004-637X-

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