The Dynamic Evolution of Multipoint Interplanetary Coronal Mass Ejections Observed with BepiColombo, Tianwen-1, and MAVEN
We present two multipoint interplanetary coronal mass ejections (ICMEs) detected by the Tianwen-1 and Mars Atmosphere and Volatile Evolution spacecraft at Mars and the BepiColombo (0.56 au ∼0.67 au) upstream of Mars from 2021 December 5 to 31. This is the first time that BepiColombo is used as an up...
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| Veröffentlicht in: | Astrophysical journal. Letters 2023-07, Vol.951 (1), p.L14 |
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| creator | Chi, Yutian Shen, Chenglong Liu, Junyan Zhong, Zhihui Owens, Mathew Scott, Christopher Barnard, Luke Yu, Bingkun Heyner, Daniel Auster, Hans-Ulrich Richter, Ingo Wang, Yuming Zhang, Tielong Guo, Jingnan Sánchez-Cano, Beatriz Pan, Zonghao Zou, Zhuxuan Xu, Mengjiao Cheng, Long Su, Zhenpeng Mao, Dongwei Zhang, Zhiyong Wang, Can Wu, Zhiyong Wang, Guoqiang Xiao, Sudong Liu, Kai Hao, Xinjun Li, Yiren Chen, Manming Lockwood, Mike |
| description | We present two multipoint interplanetary coronal mass ejections (ICMEs) detected by the Tianwen-1 and Mars Atmosphere and Volatile Evolution spacecraft at Mars and the BepiColombo (0.56 au ∼0.67 au) upstream of Mars from 2021 December 5 to 31. This is the first time that BepiColombo is used as an upstream solar wind monitor ahead of Mars and that Tianwen-1 is used to investigate the magnetic field characteristics of ICMEs at Mars. The Heliospheric Upwind Extrapolation time model was used to connect the multiple in situ observations and the coronagraph observations from STEREO/SECCHI and SOHO/LASCO. The first fast coronal mass ejection event (∼761.2 km s
−1
), which erupted on December 4, impacted Mars centrally and grazed BepiColombo by its western flank. The ambient slow solar wind decelerated the west flank of the ICME, implying that the ICME event was significantly distorted by the solar wind structure. The second slow ICME event (∼390.7 km s
−1
) underwent an acceleration from its eruption to a distance within 0.69 au and then traveled with the constant velocity of the ambient solar wind. These findings highlight the importance of background solar wind in determining the interplanetary evolution and global morphology of ICMEs up to Mars distance. Observations from multiple locations are invaluable for space weather studies at Mars and merit more exploration in the future. |
| doi_str_mv | 10.3847/2041-8213/acd7e7 |
| format | Article |
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−1
), which erupted on December 4, impacted Mars centrally and grazed BepiColombo by its western flank. The ambient slow solar wind decelerated the west flank of the ICME, implying that the ICME event was significantly distorted by the solar wind structure. The second slow ICME event (∼390.7 km s
−1
) underwent an acceleration from its eruption to a distance within 0.69 au and then traveled with the constant velocity of the ambient solar wind. These findings highlight the importance of background solar wind in determining the interplanetary evolution and global morphology of ICMEs up to Mars distance. Observations from multiple locations are invaluable for space weather studies at Mars and merit more exploration in the future.</description><identifier>ISSN: 2041-8205</identifier><identifier>EISSN: 2041-8213</identifier><identifier>DOI: 10.3847/2041-8213/acd7e7</identifier><language>eng</language><publisher>Austin: The American Astronomical Society</publisher><subject>Acceleration ; Bepi Colombo (ESA) ; Coronagraphs ; Coronal mass ejection ; Deceleration ; Evolution ; Heliosphere ; Magnetic fields ; Mars ; Mars atmosphere ; Planetary magnetic fields ; Solar coronal mass ejections ; Solar wind ; Solar wind structure ; Space weather ; Spacecraft ; Upstream ; Wind structure</subject><ispartof>Astrophysical journal. Letters, 2023-07, Vol.951 (1), p.L14</ispartof><rights>2023. The Author(s). Published by the American Astronomical Society.</rights><rights>2023. The Author(s). Published by the American Astronomical Society. This work 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><citedby>FETCH-LOGICAL-c447t-1f5b4d49a2af28e9a8a37bd23848d232cc4801de559dc7ff50a8b8bc40a9aa743</citedby><cites>FETCH-LOGICAL-c447t-1f5b4d49a2af28e9a8a37bd23848d232cc4801de559dc7ff50a8b8bc40a9aa743</cites><orcidid>0000-0002-6618-4928 ; 0000-0002-8887-3919 ; 0000-0003-2061-2453 ; 0000-0001-6411-5649 ; 0000-0002-3577-5223 ; 0009-0006-7051-0438 ; 0000-0002-2924-7520 ; 0000-0003-2758-1960 ; 0009-0008-9920-9600 ; 0000-0002-5324-4039 ; 0000-0002-8707-076X ; 0000-0001-5577-4538 ; 0000-0001-9315-4487 ; 0000-0003-0578-6244 ; 0000-0001-9876-4612 ; 0000-0003-2573-1531 ; 0000-0002-5627-2377 ; 0000-0002-2865-4626 ; 0000-0003-0277-3253 ; 0000-0002-7397-2172</orcidid></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><linktopdf>$$Uhttps://iopscience.iop.org/article/10.3847/2041-8213/acd7e7/pdf$$EPDF$$P50$$Giop$$Hfree_for_read</linktopdf><link.rule.ids>314,776,780,860,2096,27901,27902,38845,38867,53815,53842</link.rule.ids></links><search><creatorcontrib>Chi, Yutian</creatorcontrib><creatorcontrib>Shen, Chenglong</creatorcontrib><creatorcontrib>Liu, Junyan</creatorcontrib><creatorcontrib>Zhong, Zhihui</creatorcontrib><creatorcontrib>Owens, Mathew</creatorcontrib><creatorcontrib>Scott, Christopher</creatorcontrib><creatorcontrib>Barnard, Luke</creatorcontrib><creatorcontrib>Yu, Bingkun</creatorcontrib><creatorcontrib>Heyner, Daniel</creatorcontrib><creatorcontrib>Auster, Hans-Ulrich</creatorcontrib><creatorcontrib>Richter, Ingo</creatorcontrib><creatorcontrib>Wang, Yuming</creatorcontrib><creatorcontrib>Zhang, Tielong</creatorcontrib><creatorcontrib>Guo, Jingnan</creatorcontrib><creatorcontrib>Sánchez-Cano, Beatriz</creatorcontrib><creatorcontrib>Pan, Zonghao</creatorcontrib><creatorcontrib>Zou, Zhuxuan</creatorcontrib><creatorcontrib>Xu, Mengjiao</creatorcontrib><creatorcontrib>Cheng, Long</creatorcontrib><creatorcontrib>Su, Zhenpeng</creatorcontrib><creatorcontrib>Mao, Dongwei</creatorcontrib><creatorcontrib>Zhang, Zhiyong</creatorcontrib><creatorcontrib>Wang, Can</creatorcontrib><creatorcontrib>Wu, Zhiyong</creatorcontrib><creatorcontrib>Wang, Guoqiang</creatorcontrib><creatorcontrib>Xiao, Sudong</creatorcontrib><creatorcontrib>Liu, Kai</creatorcontrib><creatorcontrib>Hao, Xinjun</creatorcontrib><creatorcontrib>Li, Yiren</creatorcontrib><creatorcontrib>Chen, Manming</creatorcontrib><creatorcontrib>Lockwood, Mike</creatorcontrib><title>The Dynamic Evolution of Multipoint Interplanetary Coronal Mass Ejections Observed with BepiColombo, Tianwen-1, and MAVEN</title><title>Astrophysical journal. Letters</title><addtitle>APJL</addtitle><addtitle>Astrophys. J. Lett</addtitle><description>We present two multipoint interplanetary coronal mass ejections (ICMEs) detected by the Tianwen-1 and Mars Atmosphere and Volatile Evolution spacecraft at Mars and the BepiColombo (0.56 au ∼0.67 au) upstream of Mars from 2021 December 5 to 31. This is the first time that BepiColombo is used as an upstream solar wind monitor ahead of Mars and that Tianwen-1 is used to investigate the magnetic field characteristics of ICMEs at Mars. The Heliospheric Upwind Extrapolation time model was used to connect the multiple in situ observations and the coronagraph observations from STEREO/SECCHI and SOHO/LASCO. The first fast coronal mass ejection event (∼761.2 km s
−1
), which erupted on December 4, impacted Mars centrally and grazed BepiColombo by its western flank. The ambient slow solar wind decelerated the west flank of the ICME, implying that the ICME event was significantly distorted by the solar wind structure. The second slow ICME event (∼390.7 km s
−1
) underwent an acceleration from its eruption to a distance within 0.69 au and then traveled with the constant velocity of the ambient solar wind. These findings highlight the importance of background solar wind in determining the interplanetary evolution and global morphology of ICMEs up to Mars distance. Observations from multiple locations are invaluable for space weather studies at Mars and merit more exploration in the future.</description><subject>Acceleration</subject><subject>Bepi Colombo (ESA)</subject><subject>Coronagraphs</subject><subject>Coronal mass ejection</subject><subject>Deceleration</subject><subject>Evolution</subject><subject>Heliosphere</subject><subject>Magnetic fields</subject><subject>Mars</subject><subject>Mars atmosphere</subject><subject>Planetary magnetic fields</subject><subject>Solar coronal mass ejections</subject><subject>Solar wind</subject><subject>Solar wind structure</subject><subject>Space weather</subject><subject>Spacecraft</subject><subject>Upstream</subject><subject>Wind structure</subject><issn>2041-8205</issn><issn>2041-8213</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2023</creationdate><recordtype>article</recordtype><sourceid>O3W</sourceid><sourceid>DOA</sourceid><recordid>eNp1kc1v1DAQxSMEEqVw52gJidOG2o5TO8eyXWCl3fay5WpN_EEdZe1gZ1vtf1-HVMulvXis0Xu_0cwris8Ef6sE4xcUM1IKSqoLUJob_qY4O7Xenv64fl98SKnDmOJLIs6K4-7eoOujh71TaPUQ-sPogkfBou2hH90QnB_R2o8mDj14M0I8omWIwUOPtpASWnVGTZaEbttk4oPR6NGN9-i7Gdwy9GHfhgXaOfCPxpdkgcBrtL36vbr5WLyz0Cfz6bmeF3c_Vrvlr3Jz-3O9vNqUijE-lsTWLdOsAQqWCtOAgIq3mualRX6pUkxgok1dN1pxa2sMohWtYhgaAM6q82I9c3WATg7R7fMOMoCT_xoh_pEQR6d6I8FctoJmXGVqBiyP0dhWlglCGed6Yn2ZWUMMfw8mjbILh5hvkSQVFWG0bliVVXhWqRhSisaephIsp7DklIackpFzWNnydba4MPxnwtD1sqmJJHJDmBy0zcLFC8JXuU8NkaM0</recordid><startdate>20230701</startdate><enddate>20230701</enddate><creator>Chi, Yutian</creator><creator>Shen, Chenglong</creator><creator>Liu, Junyan</creator><creator>Zhong, Zhihui</creator><creator>Owens, Mathew</creator><creator>Scott, Christopher</creator><creator>Barnard, Luke</creator><creator>Yu, Bingkun</creator><creator>Heyner, Daniel</creator><creator>Auster, Hans-Ulrich</creator><creator>Richter, Ingo</creator><creator>Wang, Yuming</creator><creator>Zhang, Tielong</creator><creator>Guo, Jingnan</creator><creator>Sánchez-Cano, Beatriz</creator><creator>Pan, Zonghao</creator><creator>Zou, Zhuxuan</creator><creator>Xu, Mengjiao</creator><creator>Cheng, Long</creator><creator>Su, Zhenpeng</creator><creator>Mao, Dongwei</creator><creator>Zhang, Zhiyong</creator><creator>Wang, Can</creator><creator>Wu, Zhiyong</creator><creator>Wang, Guoqiang</creator><creator>Xiao, Sudong</creator><creator>Liu, Kai</creator><creator>Hao, Xinjun</creator><creator>Li, Yiren</creator><creator>Chen, Manming</creator><creator>Lockwood, Mike</creator><general>The American Astronomical Society</general><general>IOP Publishing</general><scope>O3W</scope><scope>TSCCA</scope><scope>AAYXX</scope><scope>CITATION</scope><scope>7TG</scope><scope>8FD</scope><scope>H8D</scope><scope>KL.</scope><scope>L7M</scope><scope>DOA</scope><orcidid>https://orcid.org/0000-0002-6618-4928</orcidid><orcidid>https://orcid.org/0000-0002-8887-3919</orcidid><orcidid>https://orcid.org/0000-0003-2061-2453</orcidid><orcidid>https://orcid.org/0000-0001-6411-5649</orcidid><orcidid>https://orcid.org/0000-0002-3577-5223</orcidid><orcidid>https://orcid.org/0009-0006-7051-0438</orcidid><orcidid>https://orcid.org/0000-0002-2924-7520</orcidid><orcidid>https://orcid.org/0000-0003-2758-1960</orcidid><orcidid>https://orcid.org/0009-0008-9920-9600</orcidid><orcidid>https://orcid.org/0000-0002-5324-4039</orcidid><orcidid>https://orcid.org/0000-0002-8707-076X</orcidid><orcidid>https://orcid.org/0000-0001-5577-4538</orcidid><orcidid>https://orcid.org/0000-0001-9315-4487</orcidid><orcidid>https://orcid.org/0000-0003-0578-6244</orcidid><orcidid>https://orcid.org/0000-0001-9876-4612</orcidid><orcidid>https://orcid.org/0000-0003-2573-1531</orcidid><orcidid>https://orcid.org/0000-0002-5627-2377</orcidid><orcidid>https://orcid.org/0000-0002-2865-4626</orcidid><orcidid>https://orcid.org/0000-0003-0277-3253</orcidid><orcidid>https://orcid.org/0000-0002-7397-2172</orcidid></search><sort><creationdate>20230701</creationdate><title>The Dynamic Evolution of Multipoint Interplanetary Coronal Mass Ejections Observed with BepiColombo, Tianwen-1, and MAVEN</title><author>Chi, Yutian ; Shen, Chenglong ; Liu, Junyan ; Zhong, Zhihui ; Owens, Mathew ; Scott, Christopher ; Barnard, Luke ; Yu, Bingkun ; Heyner, Daniel ; Auster, Hans-Ulrich ; Richter, Ingo ; Wang, Yuming ; Zhang, Tielong ; Guo, Jingnan ; Sánchez-Cano, Beatriz ; Pan, Zonghao ; Zou, Zhuxuan ; Xu, Mengjiao ; Cheng, Long ; Su, Zhenpeng ; Mao, Dongwei ; Zhang, Zhiyong ; Wang, Can ; Wu, Zhiyong ; Wang, Guoqiang ; Xiao, Sudong ; Liu, Kai ; Hao, Xinjun ; Li, Yiren ; Chen, Manming ; Lockwood, Mike</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c447t-1f5b4d49a2af28e9a8a37bd23848d232cc4801de559dc7ff50a8b8bc40a9aa743</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2023</creationdate><topic>Acceleration</topic><topic>Bepi Colombo (ESA)</topic><topic>Coronagraphs</topic><topic>Coronal mass ejection</topic><topic>Deceleration</topic><topic>Evolution</topic><topic>Heliosphere</topic><topic>Magnetic fields</topic><topic>Mars</topic><topic>Mars atmosphere</topic><topic>Planetary magnetic fields</topic><topic>Solar coronal mass ejections</topic><topic>Solar wind</topic><topic>Solar wind structure</topic><topic>Space weather</topic><topic>Spacecraft</topic><topic>Upstream</topic><topic>Wind structure</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Chi, Yutian</creatorcontrib><creatorcontrib>Shen, Chenglong</creatorcontrib><creatorcontrib>Liu, Junyan</creatorcontrib><creatorcontrib>Zhong, Zhihui</creatorcontrib><creatorcontrib>Owens, Mathew</creatorcontrib><creatorcontrib>Scott, Christopher</creatorcontrib><creatorcontrib>Barnard, Luke</creatorcontrib><creatorcontrib>Yu, Bingkun</creatorcontrib><creatorcontrib>Heyner, Daniel</creatorcontrib><creatorcontrib>Auster, Hans-Ulrich</creatorcontrib><creatorcontrib>Richter, Ingo</creatorcontrib><creatorcontrib>Wang, Yuming</creatorcontrib><creatorcontrib>Zhang, Tielong</creatorcontrib><creatorcontrib>Guo, Jingnan</creatorcontrib><creatorcontrib>Sánchez-Cano, Beatriz</creatorcontrib><creatorcontrib>Pan, Zonghao</creatorcontrib><creatorcontrib>Zou, Zhuxuan</creatorcontrib><creatorcontrib>Xu, Mengjiao</creatorcontrib><creatorcontrib>Cheng, Long</creatorcontrib><creatorcontrib>Su, Zhenpeng</creatorcontrib><creatorcontrib>Mao, Dongwei</creatorcontrib><creatorcontrib>Zhang, Zhiyong</creatorcontrib><creatorcontrib>Wang, Can</creatorcontrib><creatorcontrib>Wu, Zhiyong</creatorcontrib><creatorcontrib>Wang, Guoqiang</creatorcontrib><creatorcontrib>Xiao, Sudong</creatorcontrib><creatorcontrib>Liu, Kai</creatorcontrib><creatorcontrib>Hao, Xinjun</creatorcontrib><creatorcontrib>Li, Yiren</creatorcontrib><creatorcontrib>Chen, Manming</creatorcontrib><creatorcontrib>Lockwood, Mike</creatorcontrib><collection>IOP Publishing Free Content</collection><collection>IOPscience (Open Access)</collection><collection>CrossRef</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><collection>DOAJ Directory of Open Access Journals</collection><jtitle>Astrophysical journal. 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Letters</jtitle><stitle>APJL</stitle><addtitle>Astrophys. J. Lett</addtitle><date>2023-07-01</date><risdate>2023</risdate><volume>951</volume><issue>1</issue><spage>L14</spage><pages>L14-</pages><issn>2041-8205</issn><eissn>2041-8213</eissn><abstract>We present two multipoint interplanetary coronal mass ejections (ICMEs) detected by the Tianwen-1 and Mars Atmosphere and Volatile Evolution spacecraft at Mars and the BepiColombo (0.56 au ∼0.67 au) upstream of Mars from 2021 December 5 to 31. This is the first time that BepiColombo is used as an upstream solar wind monitor ahead of Mars and that Tianwen-1 is used to investigate the magnetic field characteristics of ICMEs at Mars. The Heliospheric Upwind Extrapolation time model was used to connect the multiple in situ observations and the coronagraph observations from STEREO/SECCHI and SOHO/LASCO. The first fast coronal mass ejection event (∼761.2 km s
−1
), which erupted on December 4, impacted Mars centrally and grazed BepiColombo by its western flank. The ambient slow solar wind decelerated the west flank of the ICME, implying that the ICME event was significantly distorted by the solar wind structure. The second slow ICME event (∼390.7 km s
−1
) underwent an acceleration from its eruption to a distance within 0.69 au and then traveled with the constant velocity of the ambient solar wind. These findings highlight the importance of background solar wind in determining the interplanetary evolution and global morphology of ICMEs up to Mars distance. Observations from multiple locations are invaluable for space weather studies at Mars and merit more exploration in the future.</abstract><cop>Austin</cop><pub>The American Astronomical Society</pub><doi>10.3847/2041-8213/acd7e7</doi><tpages>10</tpages><orcidid>https://orcid.org/0000-0002-6618-4928</orcidid><orcidid>https://orcid.org/0000-0002-8887-3919</orcidid><orcidid>https://orcid.org/0000-0003-2061-2453</orcidid><orcidid>https://orcid.org/0000-0001-6411-5649</orcidid><orcidid>https://orcid.org/0000-0002-3577-5223</orcidid><orcidid>https://orcid.org/0009-0006-7051-0438</orcidid><orcidid>https://orcid.org/0000-0002-2924-7520</orcidid><orcidid>https://orcid.org/0000-0003-2758-1960</orcidid><orcidid>https://orcid.org/0009-0008-9920-9600</orcidid><orcidid>https://orcid.org/0000-0002-5324-4039</orcidid><orcidid>https://orcid.org/0000-0002-8707-076X</orcidid><orcidid>https://orcid.org/0000-0001-5577-4538</orcidid><orcidid>https://orcid.org/0000-0001-9315-4487</orcidid><orcidid>https://orcid.org/0000-0003-0578-6244</orcidid><orcidid>https://orcid.org/0000-0001-9876-4612</orcidid><orcidid>https://orcid.org/0000-0003-2573-1531</orcidid><orcidid>https://orcid.org/0000-0002-5627-2377</orcidid><orcidid>https://orcid.org/0000-0002-2865-4626</orcidid><orcidid>https://orcid.org/0000-0003-0277-3253</orcidid><orcidid>https://orcid.org/0000-0002-7397-2172</orcidid><oa>free_for_read</oa></addata></record> |
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| ispartof | Astrophysical journal. Letters, 2023-07, Vol.951 (1), p.L14 |
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| language | eng |
| recordid | cdi_proquest_journals_2831425943 |
| source | IOP Publishing Free Content; DOAJ Directory of Open Access Journals; Elektronische Zeitschriftenbibliothek - Frei zugängliche E-Journals; IOPscience extra; Alma/SFX Local Collection |
| subjects | Acceleration Bepi Colombo (ESA) Coronagraphs Coronal mass ejection Deceleration Evolution Heliosphere Magnetic fields Mars Mars atmosphere Planetary magnetic fields Solar coronal mass ejections Solar wind Solar wind structure Space weather Spacecraft Upstream Wind structure |
| title | The Dynamic Evolution of Multipoint Interplanetary Coronal Mass Ejections Observed with BepiColombo, Tianwen-1, and MAVEN |
| url | https://sfx.bib-bvb.de/sfx_tum?ctx_ver=Z39.88-2004&ctx_enc=info:ofi/enc:UTF-8&ctx_tim=2025-02-16T00%3A52%3A45IST&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=The%20Dynamic%20Evolution%20of%20Multipoint%20Interplanetary%20Coronal%20Mass%20Ejections%20Observed%20with%20BepiColombo,%20Tianwen-1,%20and%20MAVEN&rft.jtitle=Astrophysical%20journal.%20Letters&rft.au=Chi,%20Yutian&rft.date=2023-07-01&rft.volume=951&rft.issue=1&rft.spage=L14&rft.pages=L14-&rft.issn=2041-8205&rft.eissn=2041-8213&rft_id=info:doi/10.3847/2041-8213/acd7e7&rft_dat=%3Cproquest_cross%3E2831425943%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=2831425943&rft_id=info:pmid/&rft_doaj_id=oai_doaj_org_article_ae6b828013e54a47bdd0f3f4812477d4&rfr_iscdi=true |