Exploring Solar Wind Origins and Connecting Plasma Flows from the Parker Solar Probe to 1 au: Nonspherical Source Surface and Alfvénic Fluctuations - INSU - Institut national des sciences de l'Univers Accéder directement au contenu
Article Dans Une Revue The Astrophysical Journal Supplement Année : 2020

Exploring Solar Wind Origins and Connecting Plasma Flows from the Parker Solar Probe to 1 au: Nonspherical Source Surface and Alfvénic Fluctuations

Olga Panasenco
Raffaella D’amicis
Justin Kasper
Kelly E Korreck
Keith Goetz
David M. Malaspina
  • Fonction : Auteur
Marc Pulupa
Anthony W. Case
  • Fonction : Auteur
Davin Larson
  • Fonction : Auteur
  • PersonId : 1032833
Roberto Livi
Michael Stevens
Phyllis L Whittlesey
  • Fonction : Auteur
  • PersonId : 1068579

Résumé

The magnetic field measurements of the FIELDS instrument on the Parker Solar Probe (PSP) have shown intensities, throughout its first solar encounter, that require a very low source surface (SS) height (${R}_{\mathrm{SS}}\leqslant 1.8\,{R}_{\odot }$) to be reconciled with magnetic field measurements at the Sun via potential field extrapolation (PFSS). However, during PSP's second encounter, the situation went back to a more classic SS height (${R}_{\mathrm{SS}}\leqslant 2.5\,{R}_{\odot }$). Here we use high-resolution observations of the photospheric magnetic field (Solar Dynamics Observatory/Helioseismic and Magnetic Imager) to calculate neutral lines and boundaries of the open field regions for SS heights from 1.2 to 2.5 R⊙ using an evolving PFSS model and the measured solar wind speed to trace the source of the wind observed by PSP to the low corona and photosphere. We adjust RSS to get the best match for the field polarity over the period 2018 October–November and 2019 March–April, finding that the best fit for the observed magnetic field polarity inversions requires a nonspherical SS. The geometry of the coronal hole boundaries for different RSS is tested using the PSP perihelion passes, 3D PFSS models, and LASCO/C2 observations. We investigate the sources of stronger-than-average magnetic fields and times of Alfvénic fast and slow wind. Only some of the strongly Alfvénic slow wind streams seen by PSP survive and are observed at 1 au: the origins and peculiar topology of the background in which they propagate is discussed.

Dates et versions

insu-02942565 , version 1 (18-09-2020)

Identifiants

Citer

Olga Panasenco, Marco Velli, Raffaella D’amicis, Chen Shi, Victor Réville, et al.. Exploring Solar Wind Origins and Connecting Plasma Flows from the Parker Solar Probe to 1 au: Nonspherical Source Surface and Alfvénic Fluctuations. The Astrophysical Journal Supplement, 2020, 246 (2), pp.54. ⟨10.3847/1538-4365/ab61f4⟩. ⟨insu-02942565⟩
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