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1. Identity statement
Reference TypeJournal Article
Sitemtc-m21d.sid.inpe.br
Holder Codeisadg {BR SPINPE} ibi 8JMKD3MGPCW/3DT298S
Identifier8JMKD3MGP3W34T/48L3R6S
Repositorysid.inpe.br/mtc-m21d/2023/03.02.15.49
Metadata Repositorysid.inpe.br/mtc-m21d/2023/03.02.15.49.50
Metadata Last Update2024:01.02.17.16.40 (UTC) administrator
DOI10.1038/s41550-022-01818-5
ISSN2397-3366
Citation KeyWangWaLuLiLuGo:2023:DiObTu
TitleDirect observation of turbulent magnetic reconnection in the solar wind
Year2023
MonthJan.
Access Date2024, May 19
Type of Workjournal article
Secondary TypePRE PI
2. Context
Author1 Wang, Rongsheng
2 Wang, Shimou
3 Lu, Quanming
4 Li, Xinmin
5 Lu, San
6 Gonzalez Alarcon, Walter Demétrio
Resume Identifier1
2
3
4
5
6 8JMKD3MGP5W/3C9JJC4
Group1
2
3
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6 DIHPA-CGCE-INPE-MCTI-GOV-BR
Affiliation1 University of Science and Technology of China
2 University of Science and Technology of China
3 University of Science and Technology of China
4 University of Science and Technology of China
5 University of Science and Technology of China
6 Instituto Nacional de Pesquisas Espaciais (INPE)
Author e-Mail Address1
2
3
4
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6 walterdgalarcon@yahoo.com
JournalNature Astronomy
Volume7
Number1
Pages18-28
History (UTC)2023-03-02 15:50:09 :: simone -> administrator :: 2023
2024-01-02 17:16:40 :: administrator -> simone :: 2023
3. Content and structure
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Transferable1
Content TypeExternal Contribution
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AbstractMagnetic reconnection in a current sheet is commonly found in astrophysical plasma environments. If it is often bursty, releasing magnetic free energy explosively, in planetary magnetospheres, it instead displays a quasi-steady state in the solar wind, where the energy is dissipated via slow-mode shocks. The reason for this difference is elusive. Here we present a direct observation of bursty and turbulent magnetic reconnection in the solar wind, with its associated exhausts bounded by a pair of slow-mode shocks. We infer that the plasma is more efficiently heated in the magnetic reconnection diffusion region than across the shocks and that the flow enhancement is much higher in the exhausts than in the area around the diffusion region. We detected 75 other, similar diffusion-region events in solar wind data between October 2017 and May 2019, suggesting that bursty reconnection in the solar wind is more common than previously thought and actively contributes to solar wind acceleration and heating.
AreaCEA
Arrangementurlib.net > BDMCI > Fonds > Produção a partir de 2021 > CGCE > Direct observation of...
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Next Higher Units8JMKD3MGPCW/46KTFK8
DisseminationSCOPUS
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