Magnetic Field Intermittency in the Solar Wind: Parker Solar Probe and SolO Observations Ranging from the Alfvén Region up to 1 AU - INSU - Institut national des sciences de l'Univers Accéder directement au contenu
Article Dans Une Revue The Astrophysical Journal Année : 2022

Magnetic Field Intermittency in the Solar Wind: Parker Solar Probe and SolO Observations Ranging from the Alfvén Region up to 1 AU

Nikos Sioulas
  • Fonction : Auteur
Zesen Huang
  • Fonction : Auteur
Marco Velli
  • Fonction : Auteur
Rohit Chhiber
  • Fonction : Auteur
Manuel E. Cuesta
  • Fonction : Auteur
Chen Shi
  • Fonction : Auteur
William H. Matthaeus
  • Fonction : Auteur
Riddhi Bandyopadhyay
  • Fonction : Auteur
Loukas Vlahos
  • Fonction : Auteur
Trevor A. Bowen
  • Fonction : Auteur
Ramiz A. Qudsi
  • Fonction : Auteur
Stuart D. Bale
  • Fonction : Auteur
Christopher J. Owen
  • Fonction : Auteur
Michael L. Stevens
  • Fonction : Auteur
Anthony Case
  • Fonction : Auteur
Justin Kasper
  • Fonction : Auteur
Davin Larson
  • Fonction : Auteur
Marc Pulupa
  • Fonction : Auteur
Roberto Livi
  • Fonction : Auteur

Résumé

Parker Solar Probe (PSP) and SolO data are utilized to investigate magnetic field intermittency in the solar wind (SW). Small-scale intermittency (20-100 d i ) is observed to radially strengthen when methods relying on higher-order moments are considered (SF q ; SDK), but no clear trend is observed at larger scales. However, lower-order moment-based methods (e.g., partial variance of increments; PVI) are deemed more appropriate for examining the evolution of the bulk of coherent structures (CSs), PVI ≥ 3. Using PVI, we observe a scale-dependent evolution in the fraction of the data set occupied by CSs, f PVI≥3. Specifically, regardless of the SW speed, a subtle increase is found in f PVI≥3 for ℓ = 20 d i , in contrast to a more pronounced radial increase in CSs observed at larger scales. Intermittency is investigated in relation to plasma parameters. Though, slower SW speed intervals exhibit higher f PVI≥6 and higher kurtosis maxima, no statistical differences are observed for f PVI≥3. Highly Alfvénic intervals display lower levels of intermittency. The anisotropy with respect to the angle between the magnetic field and SW flow, ΘVB is investigated. Intermittency is weaker at ΘVB ≍ 0° and is strengthened at larger angles. Considering the evolution at a constant alignment angle, a weakening of intermittency is observed with increasing advection time of the SW. Our results indicate that the strengthening of intermittency in the inner heliosphere is driven by the increase in comparatively highly intermittent perpendicular intervals sampled by the probes with increasing distance, an effect related directly to the evolution of the Parker spiral.
Fichier principal
Vignette du fichier
Sioulas_2022_ApJ_934_143.pdf (2.29 Mo) Télécharger le fichier
Origine : Fichiers éditeurs autorisés sur une archive ouverte

Dates et versions

insu-03867479 , version 1 (23-11-2022)

Licence

Paternité

Identifiants

Citer

Nikos Sioulas, Zesen Huang, Marco Velli, Rohit Chhiber, Manuel E. Cuesta, et al.. Magnetic Field Intermittency in the Solar Wind: Parker Solar Probe and SolO Observations Ranging from the Alfvén Region up to 1 AU. The Astrophysical Journal, 2022, 934, ⟨10.3847/1538-4357/ac7aa2⟩. ⟨insu-03867479⟩
32 Consultations
8 Téléchargements

Altmetric

Partager

Gmail Facebook X LinkedIn More