Formation and Evolution of the Large‐Scale Magnetic Fields in Venus' Ionosphere: Results From a Three Dimensional Global Multispecies MHD Model
Large‐scale magnetic fields have been observed in Venus' ionosphere by both the Pioneer Venus Orbiter (PVO) and Venus Express spacecraft. In this study, we examine the formation and evolution of the large‐scale magnetic field in the Venus ionosphere using a sophisticated global multispecies Mag...
Gespeichert in:
| Veröffentlicht in: | Geophysical research letters 2020-06, Vol.47 (11), p.n/a |
|---|---|
| Hauptverfasser: | , , , , |
| Format: | Artikel |
| Sprache: | eng |
| Schlagworte: | |
| Online-Zugang: | Volltext |
| Tags: |
Tag hinzufügen
Keine Tags, Fügen Sie den ersten Tag hinzu!
|
| container_end_page | n/a |
|---|---|
| container_issue | 11 |
| container_start_page | |
| container_title | Geophysical research letters |
| container_volume | 47 |
| creator | Ma, Yingjuan Toth, Gabor Nagy, Andrew Luhmann, Janet Russell, Christopher |
| description | Large‐scale magnetic fields have been observed in Venus' ionosphere by both the Pioneer Venus Orbiter (PVO) and Venus Express spacecraft. In this study, we examine the formation and evolution of the large‐scale magnetic field in the Venus ionosphere using a sophisticated global multispecies Magnetohydrodynamics (MHD) model that has been developed for Venus (Ma et al., 2013, https://doi.org/10.1029/2012JA018265). A time‐dependent model run is performed under varying solar wind dynamic pressure. Based on model results, we find that (1) the initial response of the induced magnetosphere is fast (~min), (2) a large‐scale magnetic field gradually forms in the ionosphere when the solar wind dynamic pressure suddenly exceeds the ionospheric thermal pressure, (3) both the penetration and decay of the large‐scale magnetic field in the ionosphere are slow (~hr), and (4) the ion escape rate has a nonlinear response to the change of solar wind dynamic pressure.
Plain language Summary
Large‐scale magnetic fields have been observed at Venus' ionosphere by previous Venus missions. In this study, we examine the formation and evolution of the large‐scale magnetic field in the Venus ionosphere using a sophisticated global model. A time‐dependent model run is performed under varying solar wind dynamic pressure (density). Model results show that the outside interaction region responds quickly (~min) to the solar wind variation, while the response time of the ionosphere is long (~hr). We also found that the ion escape rate has a nonlinear response to the change of solar wind dynamic pressure.
Key Points
The global MHD model self‐consistently reproduces the formation and evolution of the large‐scale magnetic fields in the Venus ionosphere
Model results show that it takes quite long time (~hr) for the magnetic field to penetrate into and decay in the ionosphere
The large‐scale magnetic fields in the ionosphere act as an additional obstacle to the solar wind |
| doi_str_mv | 10.1029/2020GL087593 |
| format | Article |
| fullrecord | <record><control><sourceid>proquest_cross</sourceid><recordid>TN_cdi_proquest_journals_2413222309</recordid><sourceformat>XML</sourceformat><sourcesystem>PC</sourcesystem><sourcerecordid>2413222309</sourcerecordid><originalsourceid>FETCH-LOGICAL-c4106-afcf42c0e067fcb281650725ddc3087736cf02d585ee691aad4e8c17a118e9bc3</originalsourceid><addsrcrecordid>eNp9kMtKAzEUhoMoWC87H-CACzdWT5K5uhNrqzBF8LYd0swZG0knNZlR3PkI-oo-iaN14crV_x_4-Dl8jO1xPOIo8mOBAicFZmmcyzU24HkUDTPEdJ0NEPO-izTZZFshPCKiRMkH7GPs_EK1xjWgmgrOn53tfi5XQzsnKJR_oM-39xutLMFUPTTUGg1jQ7YKYBq4p6YLB3DpGheWc_J0AtcUOtsGGHu3AAW3c08EI7OgJvTLysLEulkf054yYUnaUIDpxQimriK7wzZqZQPt_uY2uxuf355dDIuryeXZaTHUEcdkqGpdR0IjYZLWeiYynsSYiriqtOwNpDLRNYoqzmKiJOdKVRFlmqeK84zymZbbbH-1u_TuqaPQlo-u8_17oRQRl0IIiXlPHa4o7V0Inupy6c1C-deSY_ktvfwrvcfFCn8xll7_ZcvJdZFgnCfyC8LuhEQ</addsrcrecordid><sourcetype>Aggregation Database</sourcetype><iscdi>true</iscdi><recordtype>article</recordtype><pqid>2413222309</pqid></control><display><type>article</type><title>Formation and Evolution of the Large‐Scale Magnetic Fields in Venus' Ionosphere: Results From a Three Dimensional Global Multispecies MHD Model</title><source>Wiley Online Library Journals Frontfile Complete</source><source>Wiley Free Content</source><source>Wiley-Blackwell AGU Digital Library</source><source>EZB-FREE-00999 freely available EZB journals</source><creator>Ma, Yingjuan ; Toth, Gabor ; Nagy, Andrew ; Luhmann, Janet ; Russell, Christopher</creator><creatorcontrib>Ma, Yingjuan ; Toth, Gabor ; Nagy, Andrew ; Luhmann, Janet ; Russell, Christopher</creatorcontrib><description>Large‐scale magnetic fields have been observed in Venus' ionosphere by both the Pioneer Venus Orbiter (PVO) and Venus Express spacecraft. In this study, we examine the formation and evolution of the large‐scale magnetic field in the Venus ionosphere using a sophisticated global multispecies Magnetohydrodynamics (MHD) model that has been developed for Venus (Ma et al., 2013, https://doi.org/10.1029/2012JA018265). A time‐dependent model run is performed under varying solar wind dynamic pressure. Based on model results, we find that (1) the initial response of the induced magnetosphere is fast (~min), (2) a large‐scale magnetic field gradually forms in the ionosphere when the solar wind dynamic pressure suddenly exceeds the ionospheric thermal pressure, (3) both the penetration and decay of the large‐scale magnetic field in the ionosphere are slow (~hr), and (4) the ion escape rate has a nonlinear response to the change of solar wind dynamic pressure.
Plain language Summary
Large‐scale magnetic fields have been observed at Venus' ionosphere by previous Venus missions. In this study, we examine the formation and evolution of the large‐scale magnetic field in the Venus ionosphere using a sophisticated global model. A time‐dependent model run is performed under varying solar wind dynamic pressure (density). Model results show that the outside interaction region responds quickly (~min) to the solar wind variation, while the response time of the ionosphere is long (~hr). We also found that the ion escape rate has a nonlinear response to the change of solar wind dynamic pressure.
Key Points
The global MHD model self‐consistently reproduces the formation and evolution of the large‐scale magnetic fields in the Venus ionosphere
Model results show that it takes quite long time (~hr) for the magnetic field to penetrate into and decay in the ionosphere
The large‐scale magnetic fields in the ionosphere act as an additional obstacle to the solar wind</description><identifier>ISSN: 0094-8276</identifier><identifier>EISSN: 1944-8007</identifier><identifier>DOI: 10.1029/2020GL087593</identifier><language>eng</language><publisher>Washington: John Wiley & Sons, Inc</publisher><subject>Computational fluid dynamics ; Dynamic pressure ; Evolution ; Formation ; Ionosphere ; large‐scale magnetic field ; Magnetic field ; Magnetic fields ; Magnetism ; Magnetohydrodynamics ; Magnetospheres ; multi‐species MHD ; Nonlinear response ; Pioneer Venus 1 spacecraft ; Planetary magnetic fields ; Pressure ; Response time ; Saturn ; Solar wind ; Solar wind dynamics ; Spacecraft ; Three dimensional models ; Time dependence ; Venus ; Venus Express (ESA) ; Venus Ionosphere ; Wind variations</subject><ispartof>Geophysical research letters, 2020-06, Vol.47 (11), p.n/a</ispartof><rights>2020. American Geophysical Union. All Rights Reserved.</rights><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c4106-afcf42c0e067fcb281650725ddc3087736cf02d585ee691aad4e8c17a118e9bc3</citedby><cites>FETCH-LOGICAL-c4106-afcf42c0e067fcb281650725ddc3087736cf02d585ee691aad4e8c17a118e9bc3</cites><orcidid>0000-0001-8459-2100 ; 0000-0003-2584-7091 ; 0000-0003-2617-9259 ; 0000-0003-1639-8298 ; 0000-0003-0626-9353</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%2F2020GL087593$$EPDF$$P50$$Gwiley$$H</linktopdf><linktohtml>$$Uhttps://onlinelibrary.wiley.com/doi/full/10.1029%2F2020GL087593$$EHTML$$P50$$Gwiley$$H</linktohtml><link.rule.ids>314,776,780,1411,1427,11494,27903,27904,45553,45554,46388,46447,46812,46871</link.rule.ids></links><search><creatorcontrib>Ma, Yingjuan</creatorcontrib><creatorcontrib>Toth, Gabor</creatorcontrib><creatorcontrib>Nagy, Andrew</creatorcontrib><creatorcontrib>Luhmann, Janet</creatorcontrib><creatorcontrib>Russell, Christopher</creatorcontrib><title>Formation and Evolution of the Large‐Scale Magnetic Fields in Venus' Ionosphere: Results From a Three Dimensional Global Multispecies MHD Model</title><title>Geophysical research letters</title><description>Large‐scale magnetic fields have been observed in Venus' ionosphere by both the Pioneer Venus Orbiter (PVO) and Venus Express spacecraft. In this study, we examine the formation and evolution of the large‐scale magnetic field in the Venus ionosphere using a sophisticated global multispecies Magnetohydrodynamics (MHD) model that has been developed for Venus (Ma et al., 2013, https://doi.org/10.1029/2012JA018265). A time‐dependent model run is performed under varying solar wind dynamic pressure. Based on model results, we find that (1) the initial response of the induced magnetosphere is fast (~min), (2) a large‐scale magnetic field gradually forms in the ionosphere when the solar wind dynamic pressure suddenly exceeds the ionospheric thermal pressure, (3) both the penetration and decay of the large‐scale magnetic field in the ionosphere are slow (~hr), and (4) the ion escape rate has a nonlinear response to the change of solar wind dynamic pressure.
Plain language Summary
Large‐scale magnetic fields have been observed at Venus' ionosphere by previous Venus missions. In this study, we examine the formation and evolution of the large‐scale magnetic field in the Venus ionosphere using a sophisticated global model. A time‐dependent model run is performed under varying solar wind dynamic pressure (density). Model results show that the outside interaction region responds quickly (~min) to the solar wind variation, while the response time of the ionosphere is long (~hr). We also found that the ion escape rate has a nonlinear response to the change of solar wind dynamic pressure.
Key Points
The global MHD model self‐consistently reproduces the formation and evolution of the large‐scale magnetic fields in the Venus ionosphere
Model results show that it takes quite long time (~hr) for the magnetic field to penetrate into and decay in the ionosphere
The large‐scale magnetic fields in the ionosphere act as an additional obstacle to the solar wind</description><subject>Computational fluid dynamics</subject><subject>Dynamic pressure</subject><subject>Evolution</subject><subject>Formation</subject><subject>Ionosphere</subject><subject>large‐scale magnetic field</subject><subject>Magnetic field</subject><subject>Magnetic fields</subject><subject>Magnetism</subject><subject>Magnetohydrodynamics</subject><subject>Magnetospheres</subject><subject>multi‐species MHD</subject><subject>Nonlinear response</subject><subject>Pioneer Venus 1 spacecraft</subject><subject>Planetary magnetic fields</subject><subject>Pressure</subject><subject>Response time</subject><subject>Saturn</subject><subject>Solar wind</subject><subject>Solar wind dynamics</subject><subject>Spacecraft</subject><subject>Three dimensional models</subject><subject>Time dependence</subject><subject>Venus</subject><subject>Venus Express (ESA)</subject><subject>Venus Ionosphere</subject><subject>Wind variations</subject><issn>0094-8276</issn><issn>1944-8007</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2020</creationdate><recordtype>article</recordtype><recordid>eNp9kMtKAzEUhoMoWC87H-CACzdWT5K5uhNrqzBF8LYd0swZG0knNZlR3PkI-oo-iaN14crV_x_4-Dl8jO1xPOIo8mOBAicFZmmcyzU24HkUDTPEdJ0NEPO-izTZZFshPCKiRMkH7GPs_EK1xjWgmgrOn53tfi5XQzsnKJR_oM-39xutLMFUPTTUGg1jQ7YKYBq4p6YLB3DpGheWc_J0AtcUOtsGGHu3AAW3c08EI7OgJvTLysLEulkf054yYUnaUIDpxQimriK7wzZqZQPt_uY2uxuf355dDIuryeXZaTHUEcdkqGpdR0IjYZLWeiYynsSYiriqtOwNpDLRNYoqzmKiJOdKVRFlmqeK84zymZbbbH-1u_TuqaPQlo-u8_17oRQRl0IIiXlPHa4o7V0Inupy6c1C-deSY_ktvfwrvcfFCn8xll7_ZcvJdZFgnCfyC8LuhEQ</recordid><startdate>20200616</startdate><enddate>20200616</enddate><creator>Ma, Yingjuan</creator><creator>Toth, Gabor</creator><creator>Nagy, Andrew</creator><creator>Luhmann, Janet</creator><creator>Russell, Christopher</creator><general>John Wiley & Sons, Inc</general><scope>AAYXX</scope><scope>CITATION</scope><scope>7TG</scope><scope>7TN</scope><scope>8FD</scope><scope>F1W</scope><scope>FR3</scope><scope>H8D</scope><scope>H96</scope><scope>KL.</scope><scope>KR7</scope><scope>L.G</scope><scope>L7M</scope><orcidid>https://orcid.org/0000-0001-8459-2100</orcidid><orcidid>https://orcid.org/0000-0003-2584-7091</orcidid><orcidid>https://orcid.org/0000-0003-2617-9259</orcidid><orcidid>https://orcid.org/0000-0003-1639-8298</orcidid><orcidid>https://orcid.org/0000-0003-0626-9353</orcidid></search><sort><creationdate>20200616</creationdate><title>Formation and Evolution of the Large‐Scale Magnetic Fields in Venus' Ionosphere: Results From a Three Dimensional Global Multispecies MHD Model</title><author>Ma, Yingjuan ; Toth, Gabor ; Nagy, Andrew ; Luhmann, Janet ; Russell, Christopher</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c4106-afcf42c0e067fcb281650725ddc3087736cf02d585ee691aad4e8c17a118e9bc3</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2020</creationdate><topic>Computational fluid dynamics</topic><topic>Dynamic pressure</topic><topic>Evolution</topic><topic>Formation</topic><topic>Ionosphere</topic><topic>large‐scale magnetic field</topic><topic>Magnetic field</topic><topic>Magnetic fields</topic><topic>Magnetism</topic><topic>Magnetohydrodynamics</topic><topic>Magnetospheres</topic><topic>multi‐species MHD</topic><topic>Nonlinear response</topic><topic>Pioneer Venus 1 spacecraft</topic><topic>Planetary magnetic fields</topic><topic>Pressure</topic><topic>Response time</topic><topic>Saturn</topic><topic>Solar wind</topic><topic>Solar wind dynamics</topic><topic>Spacecraft</topic><topic>Three dimensional models</topic><topic>Time dependence</topic><topic>Venus</topic><topic>Venus Express (ESA)</topic><topic>Venus Ionosphere</topic><topic>Wind variations</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Ma, Yingjuan</creatorcontrib><creatorcontrib>Toth, Gabor</creatorcontrib><creatorcontrib>Nagy, Andrew</creatorcontrib><creatorcontrib>Luhmann, Janet</creatorcontrib><creatorcontrib>Russell, Christopher</creatorcontrib><collection>CrossRef</collection><collection>Meteorological & Geoastrophysical Abstracts</collection><collection>Oceanic Abstracts</collection><collection>Technology Research Database</collection><collection>ASFA: Aquatic Sciences and Fisheries Abstracts</collection><collection>Engineering Research Database</collection><collection>Aerospace Database</collection><collection>Aquatic Science & Fisheries Abstracts (ASFA) 2: Ocean Technology, Policy & Non-Living Resources</collection><collection>Meteorological & Geoastrophysical Abstracts - Academic</collection><collection>Civil Engineering Abstracts</collection><collection>Aquatic Science & Fisheries Abstracts (ASFA) Professional</collection><collection>Advanced Technologies Database with Aerospace</collection><jtitle>Geophysical research letters</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Ma, Yingjuan</au><au>Toth, Gabor</au><au>Nagy, Andrew</au><au>Luhmann, Janet</au><au>Russell, Christopher</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Formation and Evolution of the Large‐Scale Magnetic Fields in Venus' Ionosphere: Results From a Three Dimensional Global Multispecies MHD Model</atitle><jtitle>Geophysical research letters</jtitle><date>2020-06-16</date><risdate>2020</risdate><volume>47</volume><issue>11</issue><epage>n/a</epage><issn>0094-8276</issn><eissn>1944-8007</eissn><abstract>Large‐scale magnetic fields have been observed in Venus' ionosphere by both the Pioneer Venus Orbiter (PVO) and Venus Express spacecraft. In this study, we examine the formation and evolution of the large‐scale magnetic field in the Venus ionosphere using a sophisticated global multispecies Magnetohydrodynamics (MHD) model that has been developed for Venus (Ma et al., 2013, https://doi.org/10.1029/2012JA018265). A time‐dependent model run is performed under varying solar wind dynamic pressure. Based on model results, we find that (1) the initial response of the induced magnetosphere is fast (~min), (2) a large‐scale magnetic field gradually forms in the ionosphere when the solar wind dynamic pressure suddenly exceeds the ionospheric thermal pressure, (3) both the penetration and decay of the large‐scale magnetic field in the ionosphere are slow (~hr), and (4) the ion escape rate has a nonlinear response to the change of solar wind dynamic pressure.
Plain language Summary
Large‐scale magnetic fields have been observed at Venus' ionosphere by previous Venus missions. In this study, we examine the formation and evolution of the large‐scale magnetic field in the Venus ionosphere using a sophisticated global model. A time‐dependent model run is performed under varying solar wind dynamic pressure (density). Model results show that the outside interaction region responds quickly (~min) to the solar wind variation, while the response time of the ionosphere is long (~hr). We also found that the ion escape rate has a nonlinear response to the change of solar wind dynamic pressure.
Key Points
The global MHD model self‐consistently reproduces the formation and evolution of the large‐scale magnetic fields in the Venus ionosphere
Model results show that it takes quite long time (~hr) for the magnetic field to penetrate into and decay in the ionosphere
The large‐scale magnetic fields in the ionosphere act as an additional obstacle to the solar wind</abstract><cop>Washington</cop><pub>John Wiley & Sons, Inc</pub><doi>10.1029/2020GL087593</doi><tpages>10</tpages><orcidid>https://orcid.org/0000-0001-8459-2100</orcidid><orcidid>https://orcid.org/0000-0003-2584-7091</orcidid><orcidid>https://orcid.org/0000-0003-2617-9259</orcidid><orcidid>https://orcid.org/0000-0003-1639-8298</orcidid><orcidid>https://orcid.org/0000-0003-0626-9353</orcidid><oa>free_for_read</oa></addata></record> |
| fulltext | fulltext |
| identifier | ISSN: 0094-8276 |
| ispartof | Geophysical research letters, 2020-06, Vol.47 (11), p.n/a |
| issn | 0094-8276 1944-8007 |
| language | eng |
| recordid | cdi_proquest_journals_2413222309 |
| source | Wiley Online Library Journals Frontfile Complete; Wiley Free Content; Wiley-Blackwell AGU Digital Library; EZB-FREE-00999 freely available EZB journals |
| subjects | Computational fluid dynamics Dynamic pressure Evolution Formation Ionosphere large‐scale magnetic field Magnetic field Magnetic fields Magnetism Magnetohydrodynamics Magnetospheres multi‐species MHD Nonlinear response Pioneer Venus 1 spacecraft Planetary magnetic fields Pressure Response time Saturn Solar wind Solar wind dynamics Spacecraft Three dimensional models Time dependence Venus Venus Express (ESA) Venus Ionosphere Wind variations |
| title | Formation and Evolution of the Large‐Scale Magnetic Fields in Venus' Ionosphere: Results From a Three Dimensional Global Multispecies MHD Model |
| url | https://sfx.bib-bvb.de/sfx_tum?ctx_ver=Z39.88-2004&ctx_enc=info:ofi/enc:UTF-8&ctx_tim=2025-01-22T01%3A41%3A44IST&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=Formation%20and%20Evolution%20of%20the%20Large%E2%80%90Scale%20Magnetic%20Fields%20in%20Venus'%20Ionosphere:%20Results%20From%20a%20Three%20Dimensional%20Global%20Multispecies%20MHD%20Model&rft.jtitle=Geophysical%20research%20letters&rft.au=Ma,%20Yingjuan&rft.date=2020-06-16&rft.volume=47&rft.issue=11&rft.epage=n/a&rft.issn=0094-8276&rft.eissn=1944-8007&rft_id=info:doi/10.1029/2020GL087593&rft_dat=%3Cproquest_cross%3E2413222309%3C/proquest_cross%3E%3Curl%3E%3C/url%3E&disable_directlink=true&sfx.directlink=off&sfx.report_link=0&rft_id=info:oai/&rft_pqid=2413222309&rft_id=info:pmid/&rfr_iscdi=true |