The Astrophysical Journal Letters (Jan 2023)

Magnetic Field Spectral Evolution in the Inner Heliosphere

  • Nikos Sioulas,
  • Zesen Huang,
  • Chen Shi,
  • Marco Velli,
  • Anna Tenerani,
  • Trevor A. Bowen,
  • Stuart D. Bale,
  • Jia Huang,
  • Loukas Vlahos,
  • L. D. Woodham,
  • T. S. Horbury,
  • Thierry Dudok de Wit,
  • Davin Larson,
  • Justin Kasper,
  • Christopher J. Owen,
  • Michael L. Stevens,
  • Anthony Case,
  • Marc Pulupa,
  • David M. Malaspina,
  • J. W. Bonnell,
  • Roberto Livi,
  • Keith Goetz,
  • Peter R. Harvey,
  • Robert J. MacDowall,
  • Milan Maksimović,
  • P. Louarn,
  • A. Fedorov

DOI
https://doi.org/10.3847/2041-8213/acaeff
Journal volume & issue
Vol. 943, no. 1
p. L8

Abstract

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Parker Solar Probe and Solar Orbiter data are used to investigate the radial evolution of magnetic turbulence between 0.06 ≲ R ≲ 1 au. The spectrum is studied as a function of scale, normalized to the ion inertial scale d _i . In the vicinity of the Sun, the inertial range is limited to a narrow range of scales and exhibits a power-law exponent of, α _B = −3/2, independent of plasma parameters. The inertial range grows with distance, progressively extending to larger spatial scales, while steepening toward a α _B = −5/3 scaling. It is observed that spectra for intervals with large magnetic energy excesses and low Alfvénic content steepen significantly with distance, in contrast to highly Alfvénic intervals that retain their near-Sun scaling. The occurrence of steeper spectra in slower wind streams may be attributed to the observed positive correlation between solar wind speed and Alfvénicity.

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