Particle trajectories and acceleration during 3D fan reconnection
Context. The primary energy release in solar flares is almost certainly due to magnetic reconnection, making this a strong candidate as a mechanism for particle acceleration. While particle acceleration in 2D geometries has been widely studied, investigations in 3D are a recent development. Two main...
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Veröffentlicht in: | Astronomy and astrophysics (Berlin) 2008-11, Vol.491 (1), p.289-295 |
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description | Context. The primary energy release in solar flares is almost certainly due to magnetic reconnection, making this a strong candidate as a mechanism for particle acceleration. While particle acceleration in 2D geometries has been widely studied, investigations in 3D are a recent development. Two main classes of reconnection regimes at a 3D magnetic null point have been identified: fan and spine reconnection Aims. Here we investigate particle trajectories and acceleration during reconnection at a 3D null point, using a test particle numerical code, and compare the efficiency of the fan and spine regimes in generating an energetic particle population. Methods. We calculated the time evolution of the energy spectra. We discuss the geometry of particle escape from the two configurations and characterise the trapped and escaped populations. Results. We find that fan reconnection is less efficent than spine reconnection in providing seed particles to the region of strong electric field where acceleration is possible. The establishment of a steady-state spectrum requires approximately double the time in fan reconnection. The steady-state energy spectrum at intermediate energies (protons 1 keV to 0.1 MeV) is comparable in the fan and spine regimes. While in spine reconnection particle escape takes place in two symmetric jets along the spine, in fan reconnection no jets are produced and particles escape in the fan plane, in a ribbon-like structure. |
doi_str_mv | 10.1051/0004-6361:200809771 |
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K.</creator><creatorcontrib>Dalla, S. ; Browning, P. K.</creatorcontrib><description>Context. The primary energy release in solar flares is almost certainly due to magnetic reconnection, making this a strong candidate as a mechanism for particle acceleration. While particle acceleration in 2D geometries has been widely studied, investigations in 3D are a recent development. Two main classes of reconnection regimes at a 3D magnetic null point have been identified: fan and spine reconnection Aims. Here we investigate particle trajectories and acceleration during reconnection at a 3D null point, using a test particle numerical code, and compare the efficiency of the fan and spine regimes in generating an energetic particle population. Methods. We calculated the time evolution of the energy spectra. We discuss the geometry of particle escape from the two configurations and characterise the trapped and escaped populations. Results. We find that fan reconnection is less efficent than spine reconnection in providing seed particles to the region of strong electric field where acceleration is possible. The establishment of a steady-state spectrum requires approximately double the time in fan reconnection. The steady-state energy spectrum at intermediate energies (protons 1 keV to 0.1 MeV) is comparable in the fan and spine regimes. While in spine reconnection particle escape takes place in two symmetric jets along the spine, in fan reconnection no jets are produced and particles escape in the fan plane, in a ribbon-like structure.</description><identifier>ISSN: 0004-6361</identifier><identifier>EISSN: 1432-0746</identifier><identifier>DOI: 10.1051/0004-6361:200809771</identifier><identifier>CODEN: AAEJAF</identifier><language>eng</language><publisher>Les Ulis: EDP Sciences</publisher><subject>acceleration of particles ; Astronomy ; Earth, ocean, space ; Exact sciences and technology ; Sun: flares ; Sun: particle emission</subject><ispartof>Astronomy and astrophysics (Berlin), 2008-11, Vol.491 (1), p.289-295</ispartof><rights>2008 INIST-CNRS</rights><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c393t-6f2ea81a8504497bd0af2bc221378b5c020ed91245b624ff1b754d7c8d2e3d0c3</citedby><cites>FETCH-LOGICAL-c393t-6f2ea81a8504497bd0af2bc221378b5c020ed91245b624ff1b754d7c8d2e3d0c3</cites></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>314,780,784,3727,27924,27925</link.rule.ids><backlink>$$Uhttp://pascal-francis.inist.fr/vibad/index.php?action=getRecordDetail&idt=20846934$$DView record in Pascal Francis$$Hfree_for_read</backlink></links><search><creatorcontrib>Dalla, S.</creatorcontrib><creatorcontrib>Browning, P. 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We discuss the geometry of particle escape from the two configurations and characterise the trapped and escaped populations. Results. We find that fan reconnection is less efficent than spine reconnection in providing seed particles to the region of strong electric field where acceleration is possible. The establishment of a steady-state spectrum requires approximately double the time in fan reconnection. The steady-state energy spectrum at intermediate energies (protons 1 keV to 0.1 MeV) is comparable in the fan and spine regimes. While in spine reconnection particle escape takes place in two symmetric jets along the spine, in fan reconnection no jets are produced and particles escape in the fan plane, in a ribbon-like structure.</description><subject>acceleration of particles</subject><subject>Astronomy</subject><subject>Earth, ocean, space</subject><subject>Exact sciences and technology</subject><subject>Sun: flares</subject><subject>Sun: particle emission</subject><issn>0004-6361</issn><issn>1432-0746</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2008</creationdate><recordtype>article</recordtype><recordid>eNo9kE1LAzEQhoMoWKu_wMte9LY6-c56K61VoaCCoreQzSaSus3WZAv6793S0tMwzPO-DA9ClxhuMHB8CwCsFFTgOwKgoJISH6ERZpSUIJk4RqMDcYrOcl4OK8GKjtDkxaQ-2NYVfTJLZ_suBZcLE5vCWOtal0wfulg0mxTiV0FnhTexSM52MQ70cDpHJ9602V3s5xi9z-_fpo_l4vnhaTpZlJZWtC-FJ84obBQHxipZN2A8qS0hmEpVcwsEXFNhwngtCPMe15KzRlrVEEcbsHSMrne969T9bFzu9Srk4cPWRNdtsiZAhOIcBpDuQJu6nJPzep3CyqQ_jUFvdemtDL2VoQ-6htTVvt5ka1qfTLQhH6IEFBMVZQNX7riQe_d7uJv0rYWkkmsFH3qOXz8Jns60ov94angs</recordid><startdate>20081101</startdate><enddate>20081101</enddate><creator>Dalla, S.</creator><creator>Browning, P. 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K.</creatorcontrib><collection>Istex</collection><collection>Pascal-Francis</collection><collection>CrossRef</collection><collection>Meteorological & Geoastrophysical Abstracts</collection><collection>Meteorological & Geoastrophysical Abstracts - Academic</collection><jtitle>Astronomy and astrophysics (Berlin)</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Dalla, S.</au><au>Browning, P. K.</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Particle trajectories and acceleration during 3D fan reconnection</atitle><jtitle>Astronomy and astrophysics (Berlin)</jtitle><date>2008-11-01</date><risdate>2008</risdate><volume>491</volume><issue>1</issue><spage>289</spage><epage>295</epage><pages>289-295</pages><issn>0004-6361</issn><eissn>1432-0746</eissn><coden>AAEJAF</coden><abstract>Context. The primary energy release in solar flares is almost certainly due to magnetic reconnection, making this a strong candidate as a mechanism for particle acceleration. While particle acceleration in 2D geometries has been widely studied, investigations in 3D are a recent development. Two main classes of reconnection regimes at a 3D magnetic null point have been identified: fan and spine reconnection Aims. Here we investigate particle trajectories and acceleration during reconnection at a 3D null point, using a test particle numerical code, and compare the efficiency of the fan and spine regimes in generating an energetic particle population. Methods. We calculated the time evolution of the energy spectra. We discuss the geometry of particle escape from the two configurations and characterise the trapped and escaped populations. Results. We find that fan reconnection is less efficent than spine reconnection in providing seed particles to the region of strong electric field where acceleration is possible. The establishment of a steady-state spectrum requires approximately double the time in fan reconnection. The steady-state energy spectrum at intermediate energies (protons 1 keV to 0.1 MeV) is comparable in the fan and spine regimes. While in spine reconnection particle escape takes place in two symmetric jets along the spine, in fan reconnection no jets are produced and particles escape in the fan plane, in a ribbon-like structure.</abstract><cop>Les Ulis</cop><pub>EDP Sciences</pub><doi>10.1051/0004-6361:200809771</doi><tpages>7</tpages><oa>free_for_read</oa></addata></record> |
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source | Bacon EDP Sciences France Licence nationale-ISTEX-PS-Journals-PFISTEX; EDP Sciences; EZB-FREE-00999 freely available EZB journals |
subjects | acceleration of particles Astronomy Earth, ocean, space Exact sciences and technology Sun: flares Sun: particle emission |
title | Particle trajectories and acceleration during 3D fan reconnection |
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