Interplanetary Magnetic Field By Controls the Magnetopause Location
We present a statistical study of interplanetary magnetic field (IMF) effects on the magnetopause location based on nearly 15,000 magnetopause crossings identified in the THEMIS A‐E, Magion 4, Geotail, and Interball‐1 satellite data. In order to exclude the dominant controlling role of the solar win...
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| Veröffentlicht in: | Journal of geophysical research. Space physics 2023-05, Vol.128 (5), p.n/a |
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| container_title | Journal of geophysical research. Space physics |
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| creator | Aghabozorgi Nafchi, M. Němec, F. Pi, G. Němeček, Z. Šafránková, J. Grygorov, K. Šimůnek, J. |
| description | We present a statistical study of interplanetary magnetic field (IMF) effects on the magnetopause location based on nearly 15,000 magnetopause crossings identified in the THEMIS A‐E, Magion 4, Geotail, and Interball‐1 satellite data. In order to exclude the dominant controlling role of the solar wind dynamic pressure, differences between observed and empirical model magnetopause distances are analyzed. We find that the magnetopause distance is significantly controlled by the IMF clock angle, not considered in the used empirical models. Furthermore, during very low Alfvén Mach numbers (MA |
| doi_str_mv | 10.1029/2023JA031303 |
| format | Article |
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Key Points
Nearly 15,000 magnetopause crossings are used to study the influence of interplanetary magnetic field (IMF) on the magnetopause location
The orientation of IMF By component becomes significant at the times of low Alfvén Mach number, introducing a dawn‐dusk asymmetry
Magnetopause distances are larger in the IMF direction, consistently with available magnetohydrodynamic simulations</description><identifier>ISSN: 2169-9380</identifier><identifier>EISSN: 2169-9402</identifier><identifier>DOI: 10.1029/2023JA031303</identifier><language>eng</language><publisher>Washington: Blackwell Publishing Ltd</publisher><subject>Dynamic pressure ; Empirical analysis ; empirical model ; Empirical models ; IMF ; Interplanetary magnetic field ; Mach number ; Magnetic fields ; Magnetopause ; Modelling ; Satellite data ; Saturn ; Solar wind</subject><ispartof>Journal of geophysical research. Space physics, 2023-05, Vol.128 (5), p.n/a</ispartof><rights>2023. The Authors.</rights><rights>2023. This article 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><orcidid>0000-0002-6039-3622 ; 0000-0003-4178-5206 ; 0000-0002-3233-2718 ; 0000-0003-4831-2452 ; 0000-0002-8160-3051 ; 0000-0001-9220-3902</orcidid></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><linktopdf>$$Uhttps://onlinelibrary.wiley.com/doi/pdf/10.1029%2F2023JA031303$$EPDF$$P50$$Gwiley$$Hfree_for_read</linktopdf><linktohtml>$$Uhttps://onlinelibrary.wiley.com/doi/full/10.1029%2F2023JA031303$$EHTML$$P50$$Gwiley$$Hfree_for_read</linktohtml><link.rule.ids>314,776,780,1411,27901,27902,45550,45551</link.rule.ids></links><search><creatorcontrib>Aghabozorgi Nafchi, M.</creatorcontrib><creatorcontrib>Němec, F.</creatorcontrib><creatorcontrib>Pi, G.</creatorcontrib><creatorcontrib>Němeček, Z.</creatorcontrib><creatorcontrib>Šafránková, J.</creatorcontrib><creatorcontrib>Grygorov, K.</creatorcontrib><creatorcontrib>Šimůnek, J.</creatorcontrib><title>Interplanetary Magnetic Field By Controls the Magnetopause Location</title><title>Journal of geophysical research. Space physics</title><description>We present a statistical study of interplanetary magnetic field (IMF) effects on the magnetopause location based on nearly 15,000 magnetopause crossings identified in the THEMIS A‐E, Magion 4, Geotail, and Interball‐1 satellite data. In order to exclude the dominant controlling role of the solar wind dynamic pressure, differences between observed and empirical model magnetopause distances are analyzed. We find that the magnetopause distance is significantly controlled by the IMF clock angle, not considered in the used empirical models. Furthermore, during very low Alfvén Mach numbers (MA < 4), IMF By component can induce a considerable dawn‐dusk asymmetry of the magnetopause shape. The magnetopause distance is found to be larger in the direction of the IMF vector, that is, not only the magnitude but also the orientation of the IMF By component is eventually important. The obtained results are qualitatively consistent with a magnetohydrodynamic model run at the Community Coordinated Modeling Center.
Key Points
Nearly 15,000 magnetopause crossings are used to study the influence of interplanetary magnetic field (IMF) on the magnetopause location
The orientation of IMF By component becomes significant at the times of low Alfvén Mach number, introducing a dawn‐dusk asymmetry
Magnetopause distances are larger in the IMF direction, consistently with available magnetohydrodynamic simulations</description><subject>Dynamic pressure</subject><subject>Empirical analysis</subject><subject>empirical model</subject><subject>Empirical models</subject><subject>IMF</subject><subject>Interplanetary magnetic field</subject><subject>Mach number</subject><subject>Magnetic fields</subject><subject>Magnetopause</subject><subject>Modelling</subject><subject>Satellite data</subject><subject>Saturn</subject><subject>Solar wind</subject><issn>2169-9380</issn><issn>2169-9402</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2023</creationdate><recordtype>article</recordtype><sourceid>24P</sourceid><recordid>eNpNUNFKw0AQPETBUvvmBwR8ju7eJXfZxxhsbakIos_H9XLRlJiLSYrk7z1pBZeBHWaHXXYYu0a4ReB0x4GLTQ4CBYgzNuMoKaYE-PkfFxlcssUw7CFUFiRMZ6xYt6Pru8a0bjT9FD2Z98BqGy1r15TR_RQVvh173wzR-OFOY9-Zw-CirbdmrH17xS4q0wxucepz9rZ8eC0e4-3zal3k27jjMsXYoqvISpHSDlUlFQFZqoSBBIik5SVYRFEqW4K0WbZziTS8EoKDCnAk5uzmuLfr_dfBDaPe-0PfhpOaZ5iplKRMgkscXd914ybd9fVneEwj6N-Y9P-Y9Gb1kqdKEYofKX9aUg</recordid><startdate>202305</startdate><enddate>202305</enddate><creator>Aghabozorgi Nafchi, M.</creator><creator>Němec, F.</creator><creator>Pi, G.</creator><creator>Němeček, Z.</creator><creator>Šafránková, J.</creator><creator>Grygorov, K.</creator><creator>Šimůnek, J.</creator><general>Blackwell Publishing Ltd</general><scope>24P</scope><scope>7TG</scope><scope>8FD</scope><scope>H8D</scope><scope>KL.</scope><scope>L7M</scope><orcidid>https://orcid.org/0000-0002-6039-3622</orcidid><orcidid>https://orcid.org/0000-0003-4178-5206</orcidid><orcidid>https://orcid.org/0000-0002-3233-2718</orcidid><orcidid>https://orcid.org/0000-0003-4831-2452</orcidid><orcidid>https://orcid.org/0000-0002-8160-3051</orcidid><orcidid>https://orcid.org/0000-0001-9220-3902</orcidid></search><sort><creationdate>202305</creationdate><title>Interplanetary Magnetic Field By Controls the Magnetopause Location</title><author>Aghabozorgi Nafchi, M. ; Němec, F. ; Pi, G. ; Němeček, Z. ; Šafránková, J. ; Grygorov, K. ; Šimůnek, J.</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-p2651-c1ef9c6359b17f67909c9f3a040996c2d0c113d7cd06c88be46a2f33207207e93</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2023</creationdate><topic>Dynamic pressure</topic><topic>Empirical analysis</topic><topic>empirical model</topic><topic>Empirical models</topic><topic>IMF</topic><topic>Interplanetary magnetic field</topic><topic>Mach number</topic><topic>Magnetic fields</topic><topic>Magnetopause</topic><topic>Modelling</topic><topic>Satellite data</topic><topic>Saturn</topic><topic>Solar wind</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Aghabozorgi Nafchi, M.</creatorcontrib><creatorcontrib>Němec, F.</creatorcontrib><creatorcontrib>Pi, G.</creatorcontrib><creatorcontrib>Němeček, Z.</creatorcontrib><creatorcontrib>Šafránková, J.</creatorcontrib><creatorcontrib>Grygorov, K.</creatorcontrib><creatorcontrib>Šimůnek, J.</creatorcontrib><collection>Wiley Online Library Open Access</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><jtitle>Journal of geophysical research. Space physics</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Aghabozorgi Nafchi, M.</au><au>Němec, F.</au><au>Pi, G.</au><au>Němeček, Z.</au><au>Šafránková, J.</au><au>Grygorov, K.</au><au>Šimůnek, J.</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Interplanetary Magnetic Field By Controls the Magnetopause Location</atitle><jtitle>Journal of geophysical research. Space physics</jtitle><date>2023-05</date><risdate>2023</risdate><volume>128</volume><issue>5</issue><epage>n/a</epage><issn>2169-9380</issn><eissn>2169-9402</eissn><abstract>We present a statistical study of interplanetary magnetic field (IMF) effects on the magnetopause location based on nearly 15,000 magnetopause crossings identified in the THEMIS A‐E, Magion 4, Geotail, and Interball‐1 satellite data. In order to exclude the dominant controlling role of the solar wind dynamic pressure, differences between observed and empirical model magnetopause distances are analyzed. We find that the magnetopause distance is significantly controlled by the IMF clock angle, not considered in the used empirical models. Furthermore, during very low Alfvén Mach numbers (MA < 4), IMF By component can induce a considerable dawn‐dusk asymmetry of the magnetopause shape. The magnetopause distance is found to be larger in the direction of the IMF vector, that is, not only the magnitude but also the orientation of the IMF By component is eventually important. The obtained results are qualitatively consistent with a magnetohydrodynamic model run at the Community Coordinated Modeling Center.
Key Points
Nearly 15,000 magnetopause crossings are used to study the influence of interplanetary magnetic field (IMF) on the magnetopause location
The orientation of IMF By component becomes significant at the times of low Alfvén Mach number, introducing a dawn‐dusk asymmetry
Magnetopause distances are larger in the IMF direction, consistently with available magnetohydrodynamic simulations</abstract><cop>Washington</cop><pub>Blackwell Publishing Ltd</pub><doi>10.1029/2023JA031303</doi><tpages>8</tpages><orcidid>https://orcid.org/0000-0002-6039-3622</orcidid><orcidid>https://orcid.org/0000-0003-4178-5206</orcidid><orcidid>https://orcid.org/0000-0002-3233-2718</orcidid><orcidid>https://orcid.org/0000-0003-4831-2452</orcidid><orcidid>https://orcid.org/0000-0002-8160-3051</orcidid><orcidid>https://orcid.org/0000-0001-9220-3902</orcidid><oa>free_for_read</oa></addata></record> |
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| subjects | Dynamic pressure Empirical analysis empirical model Empirical models IMF Interplanetary magnetic field Mach number Magnetic fields Magnetopause Modelling Satellite data Saturn Solar wind |
| title | Interplanetary Magnetic Field By Controls the Magnetopause Location |
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