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Parker Solar Probe Enters the Magnetically Dominated Solar Corona.
Kasper, J C; Klein, K G; Lichko, E; Huang, Jia; Chen, C H K; Badman, S T; Bonnell, J; Whittlesey, P L; Livi, R; Larson, D; Pulupa, M; Rahmati, A; Stansby, D; Korreck, K E; Stevens, M; Case, A W; Bale, S D; Maksimovic, M; Moncuquet, M; Goetz, K; Halekas, J S; Malaspina, D; Raouafi, Nour E; Szabo, A; MacDowall, R; Velli, Marco; Dudok de Wit, Thierry; Zank, G P.
Affiliation
  • Kasper JC; BWX Technologies, Inc., Washington, DC 20001, USA and Climate and Space Sciences and Engineering, University of Michigan, Ann Arbor, Michigan 48109, USA.
  • Klein KG; Lunar and Planetary Laboratory, University of Arizona, Tucson, Arizona 85719, USA.
  • Lichko E; Lunar and Planetary Laboratory, University of Arizona, Tucson, Arizona 85719, USA.
  • Huang J; Climate and Space Sciences and Engineering, University of Michigan, Ann Arbor, Michigan 48109, USA.
  • Chen CHK; Department of Physics and Astronomy, Queen Mary University of London, London E1 4NS, United Kingdom.
  • Badman ST; Space Sciences Laboratory at University of California, Berkeley, California, USA.
  • Bonnell J; Space Sciences Laboratory at University of California, Berkeley, California, USA.
  • Whittlesey PL; Space Sciences Laboratory at University of California, Berkeley, California, USA.
  • Livi R; Space Sciences Laboratory at University of California, Berkeley, California, USA.
  • Larson D; Space Sciences Laboratory at University of California, Berkeley, California, USA.
  • Pulupa M; Space Sciences Laboratory at University of California, Berkeley, California, USA.
  • Rahmati A; Space Sciences Laboratory at University of California, Berkeley, California, USA.
  • Stansby D; Mullard Space Science Laboratory, University College London, Holmbury St. Mary, Surrey RH5 6NT, United Kingdom.
  • Korreck KE; Smithsonian Astrophysical Observatory, Cambridge, Massachusetts 02138, USA.
  • Stevens M; Smithsonian Astrophysical Observatory, Cambridge, Massachusetts 02138, USA.
  • Case AW; Smithsonian Astrophysical Observatory, Cambridge, Massachusetts 02138, USA.
  • Bale SD; Physics Department, University of California, Berkeley, California 94720-7300, USA and Space Sciences Laboratory at University of California, Berkeley, California 94720-7300, USA.
  • Maksimovic M; LESIA, Observatoire de Paris, Universite PSL, CNRS, Sorbonne Universite, Universite de Paris, 5 place Jules Janssen, 92195 Meudon, France.
  • Moncuquet M; LESIA, Observatoire de Paris, Universite PSL, CNRS, Sorbonne Universite, Universite de Paris, 5 place Jules Janssen, 92195 Meudon, France.
  • Goetz K; School of Physics and Astronomy, University of Minnesota, Minneapolis, Minnesota 55455, USA.
  • Halekas JS; Department of Physics and Astronomy, University of Iowa, Iowa City, Iowa 52242, USA.
  • Malaspina D; Laboratory for Atmospheric and Space Physics, University of Colorado Boulder, Boulder, Colorado 80303, USA.
  • Raouafi NE; The Johns Hopkins Applied Physics Laboratory, Laurel, Maryland 20723, USA.
  • Szabo A; Heliospheric Physics Laboratory, NASA Goddard Space Flight Center, Greenbelt, Maryland, 20771, USA.
  • MacDowall R; Heliospheric Physics Laboratory, NASA Goddard Space Flight Center, Greenbelt, Maryland, 20771, USA.
  • Velli M; Earth Planetary and Space Sciences, UCLA, California 90095, USA.
  • Dudok de Wit T; LPC2E, CNRS and University of Orléans, Orléans, France.
  • Zank GP; Department of Space Science and Center for Space Plasma and Aeronomic Research, University of Alabama in Huntsville, Huntsville, Alabama 35805, USA.
Phys Rev Lett ; 127(25): 255101, 2021 Dec 17.
Article in En | MEDLINE | ID: mdl-35029449
ABSTRACT
The high temperatures and strong magnetic fields of the solar corona form streams of solar wind that expand through the Solar System into interstellar space. At 0933 UT on 28 April 2021 Parker Solar Probe entered the magnetized atmosphere of the Sun 13 million km above the photosphere, crossing below the Alfvén critical surface for five hours into plasma in casual contact with the Sun with an Alfvén Mach number of 0.79 and magnetic pressure dominating both ion and electron pressure. The spectrum of turbulence below the Alfvén critical surface is reported. Magnetic mapping suggests the region was a steady flow emerging on rapidly expanding coronal magnetic field lines lying above a pseudostreamer. The sub-Alfvénic nature of the flow may be due to suppressed magnetic reconnection at the base of the pseudostreamer, as evidenced by unusually low densities in this region and the magnetic mapping.
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Full text: 1 Collection: 01-internacional Database: MEDLINE Language: En Journal: Phys Rev Lett Year: 2021 Document type: Article Affiliation country: United States
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Add to My VHL
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XML
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Full text: 1 Collection: 01-internacional Database: MEDLINE Language: En Journal: Phys Rev Lett Year: 2021 Document type: Article Affiliation country: United States