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Article: Faraday rotation of the supernova remnant G296.5+10.0: Evidence for a magnetized progenitor wind
Title | Faraday rotation of the supernova remnant G296.5+10.0: Evidence for a magnetized progenitor wind |
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Authors | |
Keywords | Ism: Individual Objects (G296.5+10.0) Ism: Supernova Remnants Magnetic Fields Polarization Radio Continuum: Ism Stars: Winds, Outflows |
Issue Date | 2010 |
Publisher | Institute 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? |
Abstract | We 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 Identifier | http://hdl.handle.net/10722/180495 |
ISSN | 2023 Impact Factor: 4.8 2023 SCImago Journal Rankings: 1.905 |
ISI Accession Number ID | |
References |
DC Field | Value | Language |
---|---|---|
dc.contributor.author | Harvey-Smith, L | en_US |
dc.contributor.author | Gaensler, BM | en_US |
dc.contributor.author | Kothes, R | en_US |
dc.contributor.author | Townsend, R | en_US |
dc.contributor.author | Heald, GH | en_US |
dc.contributor.author | Ng, CY | en_US |
dc.contributor.author | Green, AJ | en_US |
dc.date.accessioned | 2013-01-28T01:38:50Z | - |
dc.date.available | 2013-01-28T01:38:50Z | - |
dc.date.issued | 2010 | en_US |
dc.identifier.citation | Astrophysical Journal, 2010, v. 712 n. 2, p. 1157-1165 | en_US |
dc.identifier.issn | 0004-637X | en_US |
dc.identifier.uri | http://hdl.handle.net/10722/180495 | - |
dc.description.abstract | We 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.language | eng | en_US |
dc.publisher | Institute of Physics Publishing Ltd. The Journal's web site is located at http://iopscience.iop.org/0004-637X | en_US |
dc.relation.ispartof | Astrophysical Journal | en_US |
dc.subject | Ism: Individual Objects (G296.5+10.0) | en_US |
dc.subject | Ism: Supernova Remnants | en_US |
dc.subject | Magnetic Fields | en_US |
dc.subject | Polarization | en_US |
dc.subject | Radio Continuum: Ism | en_US |
dc.subject | Stars: Winds, Outflows | en_US |
dc.title | Faraday rotation of the supernova remnant G296.5+10.0: Evidence for a magnetized progenitor wind | en_US |
dc.type | Article | en_US |
dc.identifier.email | Ng, CY: stephen_ng@hku.hk | en_US |
dc.identifier.authority | Ng, CY=rp01706 | en_US |
dc.description.nature | link_to_OA_fulltext | en_US |
dc.identifier.doi | 10.1088/0004-637X/712/2/1157 | en_US |
dc.identifier.scopus | eid_2-s2.0-77950238609 | en_US |
dc.relation.references | http://www.scopus.com/mlt/select.url?eid=2-s2.0-77950238609&selection=ref&src=s&origin=recordpage | en_US |
dc.identifier.volume | 712 | en_US |
dc.identifier.issue | 2 | en_US |
dc.identifier.spage | 1157 | en_US |
dc.identifier.epage | 1165 | en_US |
dc.identifier.isi | WOS:000275594600033 | - |
dc.publisher.place | United Kingdom | en_US |
dc.identifier.scopusauthorid | Harvey-Smith, L=6507971533 | en_US |
dc.identifier.scopusauthorid | Gaensler, BM=34769921200 | en_US |
dc.identifier.scopusauthorid | Kothes, R=6701406100 | en_US |
dc.identifier.scopusauthorid | Townsend, R=7202221432 | en_US |
dc.identifier.scopusauthorid | Heald, GH=14524879800 | en_US |
dc.identifier.scopusauthorid | Ng, CY=24830903500 | en_US |
dc.identifier.scopusauthorid | Green, AJ=7404024960 | en_US |
dc.customcontrol.immutable | jt 130808 | - |
dc.identifier.issnl | 0004-637X | - |