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Article: PSR J1709-4429's Proper Motion and Its Relationship to SNR G343.1–2.3

TitlePSR J1709-4429's Proper Motion and Its Relationship to SNR G343.1–2.3
Authors
KeywordsNeutron stars
Pulsars
Proper motions
Jets
Issue Date2021
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, 2021, v. 908 n. 1, p. article no. 50 How to Cite?
AbstractWe have obtained a deep (670 ks) CXO ACIS image of the remarkable pulsar wind nebula (PWN) of PSR J1709−4429, in four epochs during 2018–2019. Comparison with an archival 2004 data set provides a pulsar proper motion μ = 13 ± 3 mas yr−1 at a PA of 86° ± 9° (1σ combined statistical and systematic uncertainties), precluding birth near the center of SNR G343.1−2.3. At the pulsar's characteristic age of 17 kyr, the association can be preserved through a combination of progenitor wind, birth kick, and PWN outflow. Associated TeV emission may, however, indicate an explosion in an earlier supernova. Inter-epoch comparison of the X-ray images shows that the PWN is dynamic, but we are unable to conclusively measure flow speeds from blob motion. The pulsar has generated a radio/X-ray wind bubble, and we argue that the PWN's long narrow jets are swept back by shocked pulsar wind venting from this cavity. These jets may trace the polar magnetic field lines of the PWN flow, an interesting challenge for numerical modeling.
Persistent Identifierhttp://hdl.handle.net/10722/297289
ISSN
2020 Impact Factor: 5.874
2020 SCImago Journal Rankings: 2.376
ISI Accession Number ID

 

DC FieldValueLanguage
dc.contributor.authorde Vries, M-
dc.contributor.authorRomani, RW-
dc.contributor.authorKargaltsev, O-
dc.contributor.authorPavlov, G-
dc.contributor.authorPosselt, B-
dc.contributor.authorSlane, P-
dc.contributor.authorBucciantini, N-
dc.contributor.authorNg, CY-
dc.contributor.authorKlingler, N-
dc.date.accessioned2021-03-08T07:16:52Z-
dc.date.available2021-03-08T07:16:52Z-
dc.date.issued2021-
dc.identifier.citationThe Astrophysical Journal, 2021, v. 908 n. 1, p. article no. 50-
dc.identifier.issn0004-637X-
dc.identifier.urihttp://hdl.handle.net/10722/297289-
dc.description.abstractWe have obtained a deep (670 ks) CXO ACIS image of the remarkable pulsar wind nebula (PWN) of PSR J1709−4429, in four epochs during 2018–2019. Comparison with an archival 2004 data set provides a pulsar proper motion μ = 13 ± 3 mas yr−1 at a PA of 86° ± 9° (1σ combined statistical and systematic uncertainties), precluding birth near the center of SNR G343.1−2.3. At the pulsar's characteristic age of 17 kyr, the association can be preserved through a combination of progenitor wind, birth kick, and PWN outflow. Associated TeV emission may, however, indicate an explosion in an earlier supernova. Inter-epoch comparison of the X-ray images shows that the PWN is dynamic, but we are unable to conclusively measure flow speeds from blob motion. The pulsar has generated a radio/X-ray wind bubble, and we argue that the PWN's long narrow jets are swept back by shocked pulsar wind venting from this cavity. These jets may trace the polar magnetic field lines of the PWN flow, an interesting challenge for numerical modeling.-
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 © IOP Publishing.-
dc.subjectNeutron stars-
dc.subjectPulsars-
dc.subjectProper motions-
dc.subjectJets-
dc.titlePSR J1709-4429's Proper Motion and Its Relationship to SNR G343.1–2.3-
dc.typeArticle-
dc.identifier.emailNg, CY: ncy@astro.physics.hku.hk-
dc.identifier.authorityNg, CY=rp01706-
dc.description.naturelink_to_subscribed_fulltext-
dc.identifier.doi10.3847/1538-4357/abcebe-
dc.identifier.hkuros321664-
dc.identifier.volume908-
dc.identifier.issue1-
dc.identifier.spagearticle no. 50-
dc.identifier.epagearticle no. 50-
dc.identifier.isiWOS:000617155700001-
dc.publisher.placeUnited States-

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