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Area of Science:

  • Plasma physics
  • Astrophysics
  • Space physics

Background:

  • Collisionless turbulence dissipation is key for plasma heating and transport.
  • Understanding solar wind heating near the Sun is crucial for space weather and coronal physics.

Purpose of the Study:

  • To analyze Parker Solar Probe observations of the sub-Alfvénic solar wind.
  • To determine the primary mechanism for collisionless turbulent heating in this region.

Main Methods:

  • Analysis of in-situ Parker Solar Probe data.
  • Investigating wave-particle interactions and energy transfer processes.

Main Results:

  • Linear resonant heating by cyclotron waves does not explain observed ion energization.
  • Stochastic heating, driven by infrequent large-amplitude events, accounts for ion heating.
  • Turbulent intermittency and breaking of the proton magnetic moment are identified as key factors.

Conclusions:

  • Stochastic heating is the dominant mechanism for intermittent solar wind heating.
  • This finding has implications for understanding turbulent dissipation in the solar corona, astrophysical plasmas, and laboratory settings.