Vortex-associated reconnection for northward IMF in the Kronian magnetosphere
We have carried out a global magnetohydrodynamic simulation study of the dynamic response of Saturn's magnetosphere to northward IMF. The response can be separated into three states. Early in the simulation (state 1) vortices form on the dayside magnetopause and propagate tailward. They form fi...
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| Veröffentlicht in: | Geophysical research letters 2007-12, Vol.34 (23), p.n/a |
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| creator | Fukazawa, Keiichiro Ogino, Tatsuki Walker, Raymond J. |
| description | We have carried out a global magnetohydrodynamic simulation study of the dynamic response of Saturn's magnetosphere to northward IMF. The response can be separated into three states. Early in the simulation (state 1) vortices form on the dayside magnetopause and propagate tailward. They form first in the morning and then in the afternoon. The flows around the dawn vortices are clockwise while double vortices form at dusk with both clockwise and counterclockwise flow. The magnetopause vortices are like those associated with the Kelvin‐Helmholtz instability. Shortly after the northward IMF reaches the subsolar magnetopause reconnection begins at the equator. Later the reconnection occurs above and below the equator creating magnetic O‐regions at the magnetopause (state 2). Finally late in the simulations a series of neutral lines forms in the tail (state 3). |
| doi_str_mv | 10.1029/2007GL031784 |
| format | Article |
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Res. Lett</addtitle><description>We have carried out a global magnetohydrodynamic simulation study of the dynamic response of Saturn's magnetosphere to northward IMF. The response can be separated into three states. Early in the simulation (state 1) vortices form on the dayside magnetopause and propagate tailward. They form first in the morning and then in the afternoon. The flows around the dawn vortices are clockwise while double vortices form at dusk with both clockwise and counterclockwise flow. The magnetopause vortices are like those associated with the Kelvin‐Helmholtz instability. Shortly after the northward IMF reaches the subsolar magnetopause reconnection begins at the equator. Later the reconnection occurs above and below the equator creating magnetic O‐regions at the magnetopause (state 2). Finally late in the simulations a series of neutral lines forms in the tail (state 3).</description><subject>Earth sciences</subject><subject>Earth, ocean, space</subject><subject>Exact sciences and technology</subject><subject>magnetosphere</subject><subject>MHD simulation</subject><subject>Saturn</subject><issn>0094-8276</issn><issn>1944-8007</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2007</creationdate><recordtype>article</recordtype><recordid>eNp9kE1v1DAQhq0KpC6lN35ALuVEwB9xbB_Riv1Qs1BVBY6W40y6brP21k617b_HKKvSE6cZjZ7n1ehF6APBnwmm6gvFWCwbzIiQ1QmaEVVVpcy3N2iGsco7FfUpepfSHcaYZW6GNr9CHOGpNCkF68wIXRHBBu_Bji74og-x8BnZHkzsivVmUThfjFsoLmPwzvhiZ249jCHttxDhPXrbmyHB-XGeoZ-LbzfzVdn8WK7nX5vSVpLUZS-YZSDzn5TXmILivGuh5ZJ2ojUUOitUJaGyveSEdwL6viOWtoJxKxgj7Ax9nHL3MTw8Qhr1ziULw2A8hMekKeacKaky-GkCbQwpRej1Prqdic-aYP23M_26s4xfHHNNsmboo_HWpX-OUvl9jjNHJ-7gBnj-b6ZeXjeUSVVnqZwkl3LjL5KJ97oWTHD9-_tSLy7r1dWqUbpmfwBUAolk</recordid><startdate>20071216</startdate><enddate>20071216</enddate><creator>Fukazawa, Keiichiro</creator><creator>Ogino, Tatsuki</creator><creator>Walker, Raymond J.</creator><general>Blackwell Publishing Ltd</general><general>American Geophysical Union</general><scope>BSCLL</scope><scope>IQODW</scope><scope>AAYXX</scope><scope>CITATION</scope><scope>7TG</scope><scope>F1W</scope><scope>H96</scope><scope>KL.</scope><scope>L.G</scope></search><sort><creationdate>20071216</creationdate><title>Vortex-associated reconnection for northward IMF in the Kronian magnetosphere</title><author>Fukazawa, Keiichiro ; Ogino, Tatsuki ; Walker, Raymond J.</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c4816-f73c3e831725602e955dbeb582d7ba2edc7948e4cf8515d7effd1c2b735c73313</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2007</creationdate><topic>Earth sciences</topic><topic>Earth, ocean, space</topic><topic>Exact sciences and technology</topic><topic>magnetosphere</topic><topic>MHD simulation</topic><topic>Saturn</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Fukazawa, Keiichiro</creatorcontrib><creatorcontrib>Ogino, Tatsuki</creatorcontrib><creatorcontrib>Walker, Raymond J.</creatorcontrib><collection>Istex</collection><collection>Pascal-Francis</collection><collection>CrossRef</collection><collection>Meteorological & Geoastrophysical Abstracts</collection><collection>ASFA: Aquatic Sciences and Fisheries Abstracts</collection><collection>Aquatic Science & Fisheries Abstracts (ASFA) 2: Ocean Technology, Policy & Non-Living Resources</collection><collection>Meteorological & Geoastrophysical Abstracts - Academic</collection><collection>Aquatic Science & Fisheries Abstracts (ASFA) Professional</collection><jtitle>Geophysical research letters</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Fukazawa, Keiichiro</au><au>Ogino, Tatsuki</au><au>Walker, Raymond J.</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Vortex-associated reconnection for northward IMF in the Kronian magnetosphere</atitle><jtitle>Geophysical research letters</jtitle><addtitle>Geophys. Res. Lett</addtitle><date>2007-12-16</date><risdate>2007</risdate><volume>34</volume><issue>23</issue><epage>n/a</epage><issn>0094-8276</issn><eissn>1944-8007</eissn><coden>GPRLAJ</coden><abstract>We have carried out a global magnetohydrodynamic simulation study of the dynamic response of Saturn's magnetosphere to northward IMF. The response can be separated into three states. Early in the simulation (state 1) vortices form on the dayside magnetopause and propagate tailward. They form first in the morning and then in the afternoon. The flows around the dawn vortices are clockwise while double vortices form at dusk with both clockwise and counterclockwise flow. The magnetopause vortices are like those associated with the Kelvin‐Helmholtz instability. Shortly after the northward IMF reaches the subsolar magnetopause reconnection begins at the equator. Later the reconnection occurs above and below the equator creating magnetic O‐regions at the magnetopause (state 2). 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| source | Elektronische Zeitschriftenbibliothek - Frei zugängliche E-Journals; Wiley Free Content; Wiley-Blackwell AGU Digital Library; Wiley Online Library All Journals |
| subjects | Earth sciences Earth, ocean, space Exact sciences and technology magnetosphere MHD simulation Saturn |
| title | Vortex-associated reconnection for northward IMF in the Kronian magnetosphere |
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