Journal
ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
Volume 246, Issue 2, Pages -Publisher
IOP PUBLISHING LTD
DOI: 10.3847/1538-4365/ab4fef
Keywords
Solar wind; Solar physics; Alfven waves; Magnetohydrodynamics; Magnetohydrodynamical simulations
Categories
Funding
- NASA Parker Solar Probe Observatory Scientist grant [NNX15AF34G]
- NASA [NNN06AA01C]
- ERC SLOW_SOURCE project [SLOW_SOURCE-DLV-819189]
- GENCI supercomputers [20410133]
- National Science Foundation [ACI-1548562]
- PNST
- CNES
- IRS SpaceObs
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During Parker Solar Probe's first orbit, the solar wind plasma was observed in situ closer than ever before, the perihelion on 2018 November 6 revealing a flow that is constantly permeated by large-amplitude Alfvenic fluctuations. These include radial magnetic field reversals, or switchbacks, that seem to be a persistent feature of the young solar wind. The measurements also reveal a very strong, unexpected, azimuthal velocity component. In this work, we numerically model the solar corona during this first encounter, solving the MHD equations and accounting for Alfven wave transport and dissipation. We find that the large-scale plasma parameters are well reproduced, allowing the computation of the solar wind sources at Probe with confidence. We try to understand the dynamical nature of the solar wind to explain both the amplitude of the observed radial magnetic field and of the azimuthal velocities.
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