Loading…
Flux Pile-up Magnetic Reconnection in the Solar Photosphere
Magnetic reconnection in the temperature minimum region of the solar photosphere, observationally manifested as canceling magnetic features, is considered. Flux pile-up reconnection in the Sweet-Parker current sheet is analyzed. It is shown that the standard Sweet-Parker reconnection rate in the pho...
Saved in:
Published in: | The Astrophysical journal 2007-06, Vol.662 (2), p.1302-1308 |
---|---|
Main Authors: | , , |
Format: | Article |
Language: | English |
Subjects: | |
Citations: | Items that this one cites Items that cite this one |
Online Access: | Get full text |
Tags: |
Add Tag
No Tags, Be the first to tag this record!
|
cited_by | cdi_FETCH-LOGICAL-c410t-3610d24f729e331669f4985713de3070d6cb1f938b756b4ed73a690b586f376e3 |
---|---|
cites | cdi_FETCH-LOGICAL-c410t-3610d24f729e331669f4985713de3070d6cb1f938b756b4ed73a690b586f376e3 |
container_end_page | 1308 |
container_issue | 2 |
container_start_page | 1302 |
container_title | The Astrophysical journal |
container_volume | 662 |
creator | Litvinenko, Yuri E Chae, Jongchul Park, So-Young |
description | Magnetic reconnection in the temperature minimum region of the solar photosphere, observationally manifested as canceling magnetic features, is considered. Flux pile-up reconnection in the Sweet-Parker current sheet is analyzed. It is shown that the standard Sweet-Parker reconnection rate in the photosphere is too slow to explain the observed cancellation. Flux pile-up reconnection scalings, however, are shown to be in agreement with the speeds of canceling magnetic fragments, magnetic fields in the fragments, and the rates of magnetic flux cancellation, derived from SOHO MDI data. Pile-up factors in the range between 1 and 5 and local reconnecting magnetic fields of a few hundred G are calculated for the analyzed canceling features. The analysis shows that flux pile-up is a likely mechanism for adjusting the local parameters of reconnecting current sheets in the photosphere and for sustaining the reconnection rates that are determined by large-scale supergranular flows. The upward mass flux in the reconnection jet, associated with a large canceling feature, is predicted to exceed 10 super(15) g hr super(-1). Hence, cancellation In a few photospheric patches over several hours can lead to the formation of a solar filament in the corona. |
doi_str_mv | 10.1086/518115 |
format | article |
fullrecord | <record><control><sourceid>proquest_cross</sourceid><recordid>TN_cdi_crossref_primary_10_1086_518115</recordid><sourceformat>XML</sourceformat><sourcesystem>PC</sourcesystem><sourcerecordid>743195162</sourcerecordid><originalsourceid>FETCH-LOGICAL-c410t-3610d24f729e331669f4985713de3070d6cb1f938b756b4ed73a690b586f376e3</originalsourceid><addsrcrecordid>eNp90MtKw0AUBuBBFKxVnyEu1IVE537BlRSrQsXiBdwN08mMjaSZOJOAvr0NLRYUXB0O5-M_8ANwiOA5gpJfMCQRYltggBiROSVMbIMBhJDmnIjXXbCX0nu_YqUG4HJcdZ_ZtKxc3jXZvXmrXVva7NHZUNfOtmWos7LO2rnLnkJlYjadhzakZu6i2wc73lTJHaznELyMr59Ht_nk4eZudDXJLUWwzQlHsMDUC6wcIYhz5amSTCBSOAIFLLidIa-InAnGZ9QVghiu4IxJ7ongjgzB6Sq3ieGjc6nVizJZV1WmdqFLWlCCFEMcL-XJvxJDrjhWdANtDClF53UTy4WJXxpB3beoVy0u4fE60SRrKh9Nbcu00VIKIVgfeLZyZWh-rn3Lui9dc4411ohArJvCL_XRX_3r8zc1QIWo</addsrcrecordid><sourcetype>Aggregation Database</sourcetype><iscdi>true</iscdi><recordtype>article</recordtype><pqid>20696294</pqid></control><display><type>article</type><title>Flux Pile-up Magnetic Reconnection in the Solar Photosphere</title><source>EZB Electronic Journals Library</source><creator>Litvinenko, Yuri E ; Chae, Jongchul ; Park, So-Young</creator><creatorcontrib>Litvinenko, Yuri E ; Chae, Jongchul ; Park, So-Young</creatorcontrib><description>Magnetic reconnection in the temperature minimum region of the solar photosphere, observationally manifested as canceling magnetic features, is considered. Flux pile-up reconnection in the Sweet-Parker current sheet is analyzed. It is shown that the standard Sweet-Parker reconnection rate in the photosphere is too slow to explain the observed cancellation. Flux pile-up reconnection scalings, however, are shown to be in agreement with the speeds of canceling magnetic fragments, magnetic fields in the fragments, and the rates of magnetic flux cancellation, derived from SOHO MDI data. Pile-up factors in the range between 1 and 5 and local reconnecting magnetic fields of a few hundred G are calculated for the analyzed canceling features. The analysis shows that flux pile-up is a likely mechanism for adjusting the local parameters of reconnecting current sheets in the photosphere and for sustaining the reconnection rates that are determined by large-scale supergranular flows. The upward mass flux in the reconnection jet, associated with a large canceling feature, is predicted to exceed 10 super(15) g hr super(-1). Hence, cancellation In a few photospheric patches over several hours can lead to the formation of a solar filament in the corona.</description><identifier>ISSN: 0004-637X</identifier><identifier>EISSN: 1538-4357</identifier><identifier>DOI: 10.1086/518115</identifier><identifier>CODEN: ASJOAB</identifier><language>eng</language><publisher>Chicago, IL: IOP Publishing</publisher><subject>Astronomy ; Earth, ocean, space ; Exact sciences and technology</subject><ispartof>The Astrophysical journal, 2007-06, Vol.662 (2), p.1302-1308</ispartof><rights>2007 INIST-CNRS</rights><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c410t-3610d24f729e331669f4985713de3070d6cb1f938b756b4ed73a690b586f376e3</citedby><cites>FETCH-LOGICAL-c410t-3610d24f729e331669f4985713de3070d6cb1f938b756b4ed73a690b586f376e3</cites></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>314,776,780,27901,27902</link.rule.ids><backlink>$$Uhttp://pascal-francis.inist.fr/vibad/index.php?action=getRecordDetail&idt=18877754$$DView record in Pascal Francis$$Hfree_for_read</backlink></links><search><creatorcontrib>Litvinenko, Yuri E</creatorcontrib><creatorcontrib>Chae, Jongchul</creatorcontrib><creatorcontrib>Park, So-Young</creatorcontrib><title>Flux Pile-up Magnetic Reconnection in the Solar Photosphere</title><title>The Astrophysical journal</title><description>Magnetic reconnection in the temperature minimum region of the solar photosphere, observationally manifested as canceling magnetic features, is considered. Flux pile-up reconnection in the Sweet-Parker current sheet is analyzed. It is shown that the standard Sweet-Parker reconnection rate in the photosphere is too slow to explain the observed cancellation. Flux pile-up reconnection scalings, however, are shown to be in agreement with the speeds of canceling magnetic fragments, magnetic fields in the fragments, and the rates of magnetic flux cancellation, derived from SOHO MDI data. Pile-up factors in the range between 1 and 5 and local reconnecting magnetic fields of a few hundred G are calculated for the analyzed canceling features. The analysis shows that flux pile-up is a likely mechanism for adjusting the local parameters of reconnecting current sheets in the photosphere and for sustaining the reconnection rates that are determined by large-scale supergranular flows. The upward mass flux in the reconnection jet, associated with a large canceling feature, is predicted to exceed 10 super(15) g hr super(-1). Hence, cancellation In a few photospheric patches over several hours can lead to the formation of a solar filament in the corona.</description><subject>Astronomy</subject><subject>Earth, ocean, space</subject><subject>Exact sciences and technology</subject><issn>0004-637X</issn><issn>1538-4357</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2007</creationdate><recordtype>article</recordtype><recordid>eNp90MtKw0AUBuBBFKxVnyEu1IVE537BlRSrQsXiBdwN08mMjaSZOJOAvr0NLRYUXB0O5-M_8ANwiOA5gpJfMCQRYltggBiROSVMbIMBhJDmnIjXXbCX0nu_YqUG4HJcdZ_ZtKxc3jXZvXmrXVva7NHZUNfOtmWos7LO2rnLnkJlYjadhzakZu6i2wc73lTJHaznELyMr59Ht_nk4eZudDXJLUWwzQlHsMDUC6wcIYhz5amSTCBSOAIFLLidIa-InAnGZ9QVghiu4IxJ7ongjgzB6Sq3ieGjc6nVizJZV1WmdqFLWlCCFEMcL-XJvxJDrjhWdANtDClF53UTy4WJXxpB3beoVy0u4fE60SRrKh9Nbcu00VIKIVgfeLZyZWh-rn3Lui9dc4411ohArJvCL_XRX_3r8zc1QIWo</recordid><startdate>20070620</startdate><enddate>20070620</enddate><creator>Litvinenko, Yuri E</creator><creator>Chae, Jongchul</creator><creator>Park, So-Young</creator><general>IOP Publishing</general><general>University of Chicago Press</general><scope>IQODW</scope><scope>AAYXX</scope><scope>CITATION</scope><scope>7TG</scope><scope>KL.</scope><scope>8FD</scope><scope>H8D</scope><scope>L7M</scope></search><sort><creationdate>20070620</creationdate><title>Flux Pile-up Magnetic Reconnection in the Solar Photosphere</title><author>Litvinenko, Yuri E ; Chae, Jongchul ; Park, So-Young</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c410t-3610d24f729e331669f4985713de3070d6cb1f938b756b4ed73a690b586f376e3</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2007</creationdate><topic>Astronomy</topic><topic>Earth, ocean, space</topic><topic>Exact sciences and technology</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Litvinenko, Yuri E</creatorcontrib><creatorcontrib>Chae, Jongchul</creatorcontrib><creatorcontrib>Park, So-Young</creatorcontrib><collection>Pascal-Francis</collection><collection>CrossRef</collection><collection>Meteorological & Geoastrophysical Abstracts</collection><collection>Meteorological & Geoastrophysical Abstracts - Academic</collection><collection>Technology Research Database</collection><collection>Aerospace Database</collection><collection>Advanced Technologies Database with Aerospace</collection><jtitle>The Astrophysical journal</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Litvinenko, Yuri E</au><au>Chae, Jongchul</au><au>Park, So-Young</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Flux Pile-up Magnetic Reconnection in the Solar Photosphere</atitle><jtitle>The Astrophysical journal</jtitle><date>2007-06-20</date><risdate>2007</risdate><volume>662</volume><issue>2</issue><spage>1302</spage><epage>1308</epage><pages>1302-1308</pages><issn>0004-637X</issn><eissn>1538-4357</eissn><coden>ASJOAB</coden><abstract>Magnetic reconnection in the temperature minimum region of the solar photosphere, observationally manifested as canceling magnetic features, is considered. Flux pile-up reconnection in the Sweet-Parker current sheet is analyzed. It is shown that the standard Sweet-Parker reconnection rate in the photosphere is too slow to explain the observed cancellation. Flux pile-up reconnection scalings, however, are shown to be in agreement with the speeds of canceling magnetic fragments, magnetic fields in the fragments, and the rates of magnetic flux cancellation, derived from SOHO MDI data. Pile-up factors in the range between 1 and 5 and local reconnecting magnetic fields of a few hundred G are calculated for the analyzed canceling features. The analysis shows that flux pile-up is a likely mechanism for adjusting the local parameters of reconnecting current sheets in the photosphere and for sustaining the reconnection rates that are determined by large-scale supergranular flows. The upward mass flux in the reconnection jet, associated with a large canceling feature, is predicted to exceed 10 super(15) g hr super(-1). Hence, cancellation In a few photospheric patches over several hours can lead to the formation of a solar filament in the corona.</abstract><cop>Chicago, IL</cop><pub>IOP Publishing</pub><doi>10.1086/518115</doi><tpages>7</tpages><oa>free_for_read</oa></addata></record> |
fulltext | fulltext |
identifier | ISSN: 0004-637X |
ispartof | The Astrophysical journal, 2007-06, Vol.662 (2), p.1302-1308 |
issn | 0004-637X 1538-4357 |
language | eng |
recordid | cdi_crossref_primary_10_1086_518115 |
source | EZB Electronic Journals Library |
subjects | Astronomy Earth, ocean, space Exact sciences and technology |
title | Flux Pile-up Magnetic Reconnection in the Solar Photosphere |
url | http://sfxeu10.hosted.exlibrisgroup.com/loughborough?ctx_ver=Z39.88-2004&ctx_enc=info:ofi/enc:UTF-8&ctx_tim=2025-02-13T23%3A19%3A43IST&url_ver=Z39.88-2004&url_ctx_fmt=infofi/fmt:kev:mtx:ctx&rfr_id=info:sid/primo.exlibrisgroup.com:primo3-Article-proquest_cross&rft_val_fmt=info:ofi/fmt:kev:mtx:journal&rft.genre=article&rft.atitle=Flux%20Pile-up%20Magnetic%20Reconnection%20in%20the%20Solar%20Photosphere&rft.jtitle=The%20Astrophysical%20journal&rft.au=Litvinenko,%20Yuri%20E&rft.date=2007-06-20&rft.volume=662&rft.issue=2&rft.spage=1302&rft.epage=1308&rft.pages=1302-1308&rft.issn=0004-637X&rft.eissn=1538-4357&rft.coden=ASJOAB&rft_id=info:doi/10.1086/518115&rft_dat=%3Cproquest_cross%3E743195162%3C/proquest_cross%3E%3Cgrp_id%3Ecdi_FETCH-LOGICAL-c410t-3610d24f729e331669f4985713de3070d6cb1f938b756b4ed73a690b586f376e3%3C/grp_id%3E%3Coa%3E%3C/oa%3E%3Curl%3E%3C/url%3E&rft_id=info:oai/&rft_pqid=20696294&rft_id=info:pmid/&rfr_iscdi=true |