Rotation of Polarization Angle in Gamma-Ray Burst Prompt Phase
The rotations of the polarization angle (PA) with time (energy) can lead to the depolarization of the time-integrated (energy-integrated) polarization. However, we do not know how and when it will rotate. Here, we consider a magnetic reconnection model to investigate the polarizations, especially th...
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| Veröffentlicht in: | The Astrophysical journal 2023-03, Vol.946 (1), p.12 |
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| creator | Wang, Hao-Bing Lan, Mi-Xiang |
| description | The rotations of the polarization angle (PA) with time (energy) can lead to the depolarization of the time-integrated (energy-integrated) polarization. However, we do not know how and when it will rotate. Here, we consider a magnetic reconnection model to investigate the polarizations, especially the PA rotations of gamma-ray burst (GRB) prompt emission. For a large-scale ordered aligned magnetic field configuration, we find that within
T
50
PAs will rotate with time (energy) for slight off-axis observations. Our studies show that the rotations of the PAs are due to changes in the observed image of the emitting region before being averaged over the equal arrival time surface for the unresolved sources. We apply our model to the single-pulse bursts of GRB 170101A and GRB 170114A with time-resolved PA observations. We find it can interpret the violent PA variation of GRB 170101A, while the model could not predict the two 90° PA changes in GRB 170114A. A more detailed model should be considered. |
| doi_str_mv | 10.3847/1538-4357/acba0c |
| format | Article |
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T
50
PAs will rotate with time (energy) for slight off-axis observations. Our studies show that the rotations of the PAs are due to changes in the observed image of the emitting region before being averaged over the equal arrival time surface for the unresolved sources. We apply our model to the single-pulse bursts of GRB 170101A and GRB 170114A with time-resolved PA observations. We find it can interpret the violent PA variation of GRB 170101A, while the model could not predict the two 90° PA changes in GRB 170114A. A more detailed model should be considered.</description><identifier>ISSN: 0004-637X</identifier><identifier>EISSN: 1538-4357</identifier><identifier>DOI: 10.3847/1538-4357/acba0c</identifier><language>eng</language><publisher>Philadelphia: The American Astronomical Society</publisher><subject>Astrophysics ; Depolarization ; Gamma ray bursts ; Gamma rays ; Magnetic field configurations ; Magnetic fields ; Magnetic reconnection ; Modelling ; Polarization</subject><ispartof>The Astrophysical journal, 2023-03, Vol.946 (1), p.12</ispartof><rights>2023. The Author(s). Published by the American Astronomical Society.</rights><rights>2023. The Author(s). Published by the American Astronomical Society. This work is published under http://creativecommons.org/licenses/by/4.0/ (the “License”). Notwithstanding the ProQuest Terms and Conditions, you may use this content in accordance with the terms of the License.</rights><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c445t-575dad185e612e5feb16d3830a167570a69237601d587a12186040ab25ae61ed3</citedby><cites>FETCH-LOGICAL-c445t-575dad185e612e5feb16d3830a167570a69237601d587a12186040ab25ae61ed3</cites><orcidid>0000-0001-5641-2598</orcidid></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><linktopdf>$$Uhttps://iopscience.iop.org/article/10.3847/1538-4357/acba0c/pdf$$EPDF$$P50$$Giop$$Hfree_for_read</linktopdf><link.rule.ids>314,780,784,864,2100,27923,27924,38889,53866</link.rule.ids></links><search><creatorcontrib>Wang, Hao-Bing</creatorcontrib><creatorcontrib>Lan, Mi-Xiang</creatorcontrib><title>Rotation of Polarization Angle in Gamma-Ray Burst Prompt Phase</title><title>The Astrophysical journal</title><addtitle>APJ</addtitle><addtitle>Astrophys. J</addtitle><description>The rotations of the polarization angle (PA) with time (energy) can lead to the depolarization of the time-integrated (energy-integrated) polarization. However, we do not know how and when it will rotate. Here, we consider a magnetic reconnection model to investigate the polarizations, especially the PA rotations of gamma-ray burst (GRB) prompt emission. For a large-scale ordered aligned magnetic field configuration, we find that within
T
50
PAs will rotate with time (energy) for slight off-axis observations. Our studies show that the rotations of the PAs are due to changes in the observed image of the emitting region before being averaged over the equal arrival time surface for the unresolved sources. We apply our model to the single-pulse bursts of GRB 170101A and GRB 170114A with time-resolved PA observations. We find it can interpret the violent PA variation of GRB 170101A, while the model could not predict the two 90° PA changes in GRB 170114A. A more detailed model should be considered.</description><subject>Astrophysics</subject><subject>Depolarization</subject><subject>Gamma ray bursts</subject><subject>Gamma rays</subject><subject>Magnetic field configurations</subject><subject>Magnetic fields</subject><subject>Magnetic reconnection</subject><subject>Modelling</subject><subject>Polarization</subject><issn>0004-637X</issn><issn>1538-4357</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2023</creationdate><recordtype>article</recordtype><sourceid>O3W</sourceid><sourceid>DOA</sourceid><recordid>eNp9kM1Lw0AQxRdRsFbvHgN6NHa_d3MRatFaKFiKgrdlkuzWhKYbN-mh_vWmRupFPA1veO83w0PokuBbprkaEcF0zJlQI8hSwNkRGhxWx2iAMeaxZOrtFJ01TbmXNEkG6G7pW2gLv4m8ixZ-DaH47PV4s1rbqNhEU6gqiJewi-63oWmjRfBV3Y13aOw5OnGwbuzFzxyi18eHl8lTPH-ezibjeZxxLtpYKJFDTrSwklArnE2JzJlmGIhUQmGQCWVKYpILrYBQoiXmGFIqoEvYnA3RrOfmHkpTh6KCsDMeCvO98GFlILRFtrbGAaVWashcSjknRKc4BSqZo67jJ7hjXfWsOviPrW1aU_pt2HTvG6p0ohRLpOhcuHdlwTdNsO5wlWCzb9zs6zX7ek3feBe56SOFr3-Z_9iv_7BDXZqES0MMoabOHfsCYsmMrg</recordid><startdate>20230301</startdate><enddate>20230301</enddate><creator>Wang, Hao-Bing</creator><creator>Lan, Mi-Xiang</creator><general>The American Astronomical Society</general><general>IOP Publishing</general><scope>O3W</scope><scope>TSCCA</scope><scope>AAYXX</scope><scope>CITATION</scope><scope>7TG</scope><scope>8FD</scope><scope>H8D</scope><scope>KL.</scope><scope>L7M</scope><scope>DOA</scope><orcidid>https://orcid.org/0000-0001-5641-2598</orcidid></search><sort><creationdate>20230301</creationdate><title>Rotation of Polarization Angle in Gamma-Ray Burst Prompt Phase</title><author>Wang, Hao-Bing ; Lan, Mi-Xiang</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c445t-575dad185e612e5feb16d3830a167570a69237601d587a12186040ab25ae61ed3</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2023</creationdate><topic>Astrophysics</topic><topic>Depolarization</topic><topic>Gamma ray bursts</topic><topic>Gamma rays</topic><topic>Magnetic field configurations</topic><topic>Magnetic fields</topic><topic>Magnetic reconnection</topic><topic>Modelling</topic><topic>Polarization</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Wang, Hao-Bing</creatorcontrib><creatorcontrib>Lan, Mi-Xiang</creatorcontrib><collection>IOP Publishing Free Content</collection><collection>IOPscience (Open Access)</collection><collection>CrossRef</collection><collection>Meteorological & Geoastrophysical Abstracts</collection><collection>Technology Research Database</collection><collection>Aerospace Database</collection><collection>Meteorological & Geoastrophysical Abstracts - Academic</collection><collection>Advanced Technologies Database with Aerospace</collection><collection>DOAJ Directory of Open Access Journals</collection><jtitle>The Astrophysical journal</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Wang, Hao-Bing</au><au>Lan, Mi-Xiang</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Rotation of Polarization Angle in Gamma-Ray Burst Prompt Phase</atitle><jtitle>The Astrophysical journal</jtitle><stitle>APJ</stitle><addtitle>Astrophys. J</addtitle><date>2023-03-01</date><risdate>2023</risdate><volume>946</volume><issue>1</issue><spage>12</spage><pages>12-</pages><issn>0004-637X</issn><eissn>1538-4357</eissn><abstract>The rotations of the polarization angle (PA) with time (energy) can lead to the depolarization of the time-integrated (energy-integrated) polarization. However, we do not know how and when it will rotate. Here, we consider a magnetic reconnection model to investigate the polarizations, especially the PA rotations of gamma-ray burst (GRB) prompt emission. For a large-scale ordered aligned magnetic field configuration, we find that within
T
50
PAs will rotate with time (energy) for slight off-axis observations. Our studies show that the rotations of the PAs are due to changes in the observed image of the emitting region before being averaged over the equal arrival time surface for the unresolved sources. We apply our model to the single-pulse bursts of GRB 170101A and GRB 170114A with time-resolved PA observations. We find it can interpret the violent PA variation of GRB 170101A, while the model could not predict the two 90° PA changes in GRB 170114A. A more detailed model should be considered.</abstract><cop>Philadelphia</cop><pub>The American Astronomical Society</pub><doi>10.3847/1538-4357/acba0c</doi><tpages>10</tpages><orcidid>https://orcid.org/0000-0001-5641-2598</orcidid><oa>free_for_read</oa></addata></record> |
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| subjects | Astrophysics Depolarization Gamma ray bursts Gamma rays Magnetic field configurations Magnetic fields Magnetic reconnection Modelling Polarization |
| title | Rotation of Polarization Angle in Gamma-Ray Burst Prompt Phase |
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