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Highly structured slow solar wind emerging from an equatorial coronal hole.
Bale, S D; Badman, S T; Bonnell, J W; Bowen, T A; Burgess, D; Case, A W; Cattell, C A; Chandran, B D G; Chaston, C C; Chen, C H K; Drake, J F; de Wit, T Dudok; Eastwood, J P; Ergun, R E; Farrell, W M; Fong, C; Goetz, K; Goldstein, M; Goodrich, K A; Harvey, P R; Horbury, T S; Howes, G G; Kasper, J C; Kellogg, P J; Klimchuk, J A; Korreck, K E; Krasnoselskikh, V V; Krucker, S; Laker, R; Larson, D E; MacDowall, R J; Maksimovic, M; Malaspina, D M; Martinez-Oliveros, J; McComas, D J; Meyer-Vernet, N; Moncuquet, M; Mozer, F S; Phan, T D; Pulupa, M; Raouafi, N E; Salem, C; Stansby, D; Stevens, M; Szabo, A; Velli, M; Woolley, T; Wygant, J R.
Afiliação
  • Bale SD; Space Sciences Laboratory, University of California, Berkeley, CA, USA. bale@berkeley.edu.
  • Badman ST; Physics Department, University of California, Berkeley, CA, USA. bale@berkeley.edu.
  • Bonnell JW; The Blackett Laboratory, Imperial College London, London, UK. bale@berkeley.edu.
  • Bowen TA; School of Physics and Astronomy, Queen Mary University of London, London, UK. bale@berkeley.edu.
  • Burgess D; Space Sciences Laboratory, University of California, Berkeley, CA, USA.
  • Case AW; Physics Department, University of California, Berkeley, CA, USA.
  • Cattell CA; Space Sciences Laboratory, University of California, Berkeley, CA, USA.
  • Chandran BDG; Space Sciences Laboratory, University of California, Berkeley, CA, USA.
  • Chaston CC; School of Physics and Astronomy, Queen Mary University of London, London, UK.
  • Chen CHK; Smithsonian Astrophysical Observatory, Cambridge, MA, USA.
  • Drake JF; School of Physics and Astronomy, University of Minnesota, Minneapolis, MN, USA.
  • de Wit TD; Department of Physics & Astronomy, University of New Hampshire, Durham, NH, USA.
  • Eastwood JP; Space Science Center, University of New Hampshire, Durham, NH, USA.
  • Ergun RE; Space Sciences Laboratory, University of California, Berkeley, CA, USA.
  • Farrell WM; School of Physics and Astronomy, Queen Mary University of London, London, UK.
  • Fong C; Department of Physics, University of Maryland, College Park, MD, USA.
  • Goetz K; Institute for Physical Science and Technology, University of Maryland, College Park, MD, USA.
  • Goldstein M; Joint Space Science Institute, University of Maryland, College Park, MD, USA.
  • Goodrich KA; LPC2E, University of Orléans, CNRS, Orléans, France.
  • Harvey PR; The Blackett Laboratory, Imperial College London, London, UK.
  • Horbury TS; Laboratory for Atmospheric and Space Physics, University of Colorado, Boulder, CO, USA.
  • Howes GG; Code 695, NASA Goddard Space Flight Center, Greenbelt, MD, USA.
  • Kasper JC; Space Sciences Laboratory, University of California, Berkeley, CA, USA.
  • Kellogg PJ; Physics Department, University of California, Berkeley, CA, USA.
  • Klimchuk JA; School of Physics and Astronomy, University of Minnesota, Minneapolis, MN, USA.
  • Korreck KE; Goddard Planetary Heliophysics Institute, University of Maryland Baltimore County, Baltimore, MD, USA.
  • Krasnoselskikh VV; Code 672, NASA Goddard Space Flight Center, Greenbelt, MD, USA.
  • Krucker S; Space Sciences Laboratory, University of California, Berkeley, CA, USA.
  • Laker R; Space Sciences Laboratory, University of California, Berkeley, CA, USA.
  • Larson DE; The Blackett Laboratory, Imperial College London, London, UK.
  • MacDowall RJ; Department of Physics and Astronomy, University of Iowa, Iowa City, IA, USA.
  • Maksimovic M; Smithsonian Astrophysical Observatory, Cambridge, MA, USA.
  • Malaspina DM; Climate and Space Sciences and Engineering, University of Michigan, Ann Arbor, MI, USA.
  • Martinez-Oliveros J; School of Physics and Astronomy, University of Minnesota, Minneapolis, MN, USA.
  • McComas DJ; Heliophysics Division, NASA Goddard Space Flight Center, Greenbelt, MD, USA.
  • Meyer-Vernet N; Smithsonian Astrophysical Observatory, Cambridge, MA, USA.
  • Moncuquet M; LPC2E, University of Orléans, CNRS, Orléans, France.
  • Mozer FS; Space Sciences Laboratory, University of California, Berkeley, CA, USA.
  • Phan TD; University of Applied Sciences and Arts Northwestern Switzerland, Windisch, Switzerland.
  • Pulupa M; The Blackett Laboratory, Imperial College London, London, UK.
  • Raouafi NE; Space Sciences Laboratory, University of California, Berkeley, CA, USA.
  • Salem C; Code 695, NASA Goddard Space Flight Center, Greenbelt, MD, USA.
  • Stansby D; LESIA, Observatoire de Paris, Université PSL, Sorbonne Université, CNRS, Meudon, France.
  • Stevens M; Laboratory for Atmospheric and Space Physics, University of Colorado, Boulder, CO, USA.
  • Szabo A; Space Sciences Laboratory, University of California, Berkeley, CA, USA.
  • Velli M; Department of Astrophysical Sciences, Princeton University, Princeton, NJ, USA.
  • Woolley T; LESIA, Observatoire de Paris, Université PSL, Sorbonne Université, CNRS, Meudon, France.
  • Wygant JR; LESIA, Observatoire de Paris, Université PSL, Sorbonne Université, CNRS, Meudon, France.
Nature ; 576(7786): 237-242, 2019 12.
Article em En | MEDLINE | ID: mdl-31802007
ABSTRACT
During the solar minimum, when the Sun is at its least active, the solar wind1,2 is observed at high latitudes as a predominantly fast (more than 500 kilometres per second), highly Alfvénic rarefied stream of plasma originating from deep within coronal holes. Closer to the ecliptic plane, the solar wind is interspersed with a more variable slow wind3 of less than 500 kilometres per second. The precise origins of the slow wind streams are less certain4; theories and observations suggest that they may originate at the tips of helmet streamers5,6, from interchange reconnection near coronal hole boundaries7,8, or within coronal holes with highly diverging magnetic fields9,10. The heating mechanism required to drive the solar wind is also unresolved, although candidate mechanisms include Alfvén-wave turbulence11,12, heating by reconnection in nanoflares13, ion cyclotron wave heating14 and acceleration by thermal gradients1. At a distance of one astronomical unit, the wind is mixed and evolved, and therefore much of the diagnostic structure of these sources and processes has been lost. Here we present observations from the Parker Solar Probe15 at 36 to 54 solar radii that show evidence of slow Alfvénic solar wind emerging from a small equatorial coronal hole. The measured magnetic field exhibits patches of large, intermittent reversals that are associated with jets of plasma and enhanced Poynting flux and that are interspersed in a smoother and less turbulent flow with a near-radial magnetic field. Furthermore, plasma-wave measurements suggest the existence of electron and ion velocity-space micro-instabilities10,16 that are associated with plasma heating and thermalization processes. Our measurements suggest that there is an impulsive mechanism associated with solar-wind energization and that micro-instabilities play a part in heating, and we provide evidence that low-latitude coronal holes are a key source of the slow solar wind.
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Texto completo: 1 Coleções: 01-internacional Base de dados: MEDLINE Idioma: En Revista: Nature Ano de publicação: 2019 Tipo de documento: Article País de afiliação: Estados Unidos
Texto completo
Imprimir
XML
PubMed Links
Buscar no Google

Texto completo: 1 Coleções: 01-internacional Base de dados: MEDLINE Idioma: En Revista: Nature Ano de publicação: 2019 Tipo de documento: Article País de afiliação: Estados Unidos