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Article: Faraday rotation of the supernova remnant G296.5+10.0: Evidence for a magnetized progenitor wind

TitleFaraday rotation of the supernova remnant G296.5+10.0: Evidence for a magnetized progenitor wind
Authors
KeywordsIsm: Individual Objects (G296.5+10.0)
Ism: Supernova Remnants
Magnetic Fields
Polarization
Radio Continuum: Ism
Stars: Winds, Outflows
Issue Date2010
PublisherInstitute of Physics Publishing Ltd. The Journal's web site is located at http://iopscience.iop.org/0004-637X
Citation
Astrophysical Journal, 2010, v. 712 n. 2, p. 1157-1165 How to Cite?
AbstractWe present spectropolarimetric radio images of the supernova remnant (SNR) G296.5+10.0 at frequencies near 1.4 GHz, observed with the Australia Telescope Compact Array. By applying rotation measure (RM) synthesis to the data, a pixel-by-pixel map of Faraday rotation has been produced for the entire remnant. We find G296.5+10.0 to have a highly ordered RM structure, with mainly positive RMs (mean RM of +28 rad m-2) on the eastern side and negative RMs (mean RM of -14 rad m-2) on the western side, indicating a magnetic field which is directed away from us on one side and toward us on the other. We consider several possible mechanisms for creating the observed RM pattern. Neither Faraday rotation in foreground interstellar gas nor in a homogeneous ambient medium swept up by the SNR shell can easily explain the magnitude and sign of the observed RM pattern. Instead, we propose that the observed RMs are the imprint of an azimuthal magnetic field in the stellar wind of the progenitor star. Specifically, we calculate that a swept-up magnetized wind from a red supergiant can produce RMs of the observed magnitude, while the azimuthal pattern of the magnetic field at large distances from the star naturally produces the anti-symmetric RM pattern observed. Expansion into such a wind can possibly also account for the striking bilateral symmetry of the SNR's radio and X-ray morphologies. © 2010. The American Astronomical Society. All rights reserved..
Persistent Identifierhttp://hdl.handle.net/10722/180495
ISSN
2015 Impact Factor: 5.909
2015 SCImago Journal Rankings: 3.266
ISI Accession Number ID
References

 

DC FieldValueLanguage
dc.contributor.authorHarvey-Smith, Len_US
dc.contributor.authorGaensler, BMen_US
dc.contributor.authorKothes, Ren_US
dc.contributor.authorTownsend, Ren_US
dc.contributor.authorHeald, GHen_US
dc.contributor.authorNg, CYen_US
dc.contributor.authorGreen, AJen_US
dc.date.accessioned2013-01-28T01:38:50Z-
dc.date.available2013-01-28T01:38:50Z-
dc.date.issued2010en_US
dc.identifier.citationAstrophysical Journal, 2010, v. 712 n. 2, p. 1157-1165en_US
dc.identifier.issn0004-637Xen_US
dc.identifier.urihttp://hdl.handle.net/10722/180495-
dc.description.abstractWe present spectropolarimetric radio images of the supernova remnant (SNR) G296.5+10.0 at frequencies near 1.4 GHz, observed with the Australia Telescope Compact Array. By applying rotation measure (RM) synthesis to the data, a pixel-by-pixel map of Faraday rotation has been produced for the entire remnant. We find G296.5+10.0 to have a highly ordered RM structure, with mainly positive RMs (mean RM of +28 rad m-2) on the eastern side and negative RMs (mean RM of -14 rad m-2) on the western side, indicating a magnetic field which is directed away from us on one side and toward us on the other. We consider several possible mechanisms for creating the observed RM pattern. Neither Faraday rotation in foreground interstellar gas nor in a homogeneous ambient medium swept up by the SNR shell can easily explain the magnitude and sign of the observed RM pattern. Instead, we propose that the observed RMs are the imprint of an azimuthal magnetic field in the stellar wind of the progenitor star. Specifically, we calculate that a swept-up magnetized wind from a red supergiant can produce RMs of the observed magnitude, while the azimuthal pattern of the magnetic field at large distances from the star naturally produces the anti-symmetric RM pattern observed. Expansion into such a wind can possibly also account for the striking bilateral symmetry of the SNR's radio and X-ray morphologies. © 2010. 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/0004-637Xen_US
dc.relation.ispartofAstrophysical Journalen_US
dc.subjectIsm: Individual Objects (G296.5+10.0)en_US
dc.subjectIsm: Supernova Remnantsen_US
dc.subjectMagnetic Fieldsen_US
dc.subjectPolarizationen_US
dc.subjectRadio Continuum: Ismen_US
dc.subjectStars: Winds, Outflowsen_US
dc.titleFaraday rotation of the supernova remnant G296.5+10.0: Evidence for a magnetized progenitor winden_US
dc.typeArticleen_US
dc.identifier.emailNg, CY: stephen_ng@hku.hken_US
dc.identifier.authorityNg, CY=rp01706en_US
dc.description.naturelink_to_OA_fulltexten_US
dc.identifier.doi10.1088/0004-637X/712/2/1157en_US
dc.identifier.scopuseid_2-s2.0-77950238609en_US
dc.relation.referenceshttp://www.scopus.com/mlt/select.url?eid=2-s2.0-77950238609&selection=ref&src=s&origin=recordpageen_US
dc.identifier.volume712en_US
dc.identifier.issue2en_US
dc.identifier.spage1157en_US
dc.identifier.epage1165en_US
dc.identifier.isiWOS:000275594600033-
dc.publisher.placeUnited Kingdomen_US
dc.identifier.scopusauthoridHarvey-Smith, L=6507971533en_US
dc.identifier.scopusauthoridGaensler, BM=34769921200en_US
dc.identifier.scopusauthoridKothes, R=6701406100en_US
dc.identifier.scopusauthoridTownsend, R=7202221432en_US
dc.identifier.scopusauthoridHeald, GH=14524879800en_US
dc.identifier.scopusauthoridNg, CY=24830903500en_US
dc.identifier.scopusauthoridGreen, AJ=7404024960en_US
dc.customcontrol.immutablejt 130808-

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