The Evolution and Role of Solar Wind Turbulence in the Inner Heliosphere

TL;DR

This study analyzes Parker Solar Probe data to understand solar wind turbulence at 0.17 au, revealing increased turbulence energy, spectral similarities with velocity fields, and the role of turbulence in solar wind acceleration.

Contribution

First in situ measurements of solar wind turbulence at 0.17 au, showing its evolution and impact on solar wind energy transfer and acceleration.

Findings

Turbulence energy levels are over an order of magnitude higher at 0.17 au.

Magnetic and velocity spectral indices both approximate -3/2.

Turbulence energy flux increases significantly towards the Sun, supporting turbulence-driven solar wind models.

Abstract

The first two orbits of the Parker Solar Probe (PSP) spacecraft have enabled the first in situ measurements of the solar wind down to a heliocentric distance of 0.17 au (or 36 Rs). Here, we present an analysis of this data to study solar wind turbulence at 0.17 au and its evolution out to 1 au. While many features remain similar, key differences at 0.17 au include: increased turbulence energy levels by more than an order of magnitude, a magnetic field spectral index of -3/2 matching that of the velocity and both Elsasser fields, a lower magnetic compressibility consistent with a smaller slow-mode kinetic energy fraction, and a much smaller outer scale that has had time for substantial nonlinear processing. There is also an overall increase in the dominance of outward-propagating Alfv\'enic fluctuations compared to inward-propagating ones, and the radial variation of the inward component is consistent with its generation by reflection from the large-scale gradient in Alfv\'en speed. The energy flux in this turbulence at 0.17 au was found to be ~10% of that in the bulk solar wind kinetic energy, becoming ~40% when extrapolated to the Alfv\'en point, and both the fraction and rate of increase of this flux towards the Sun is consistent with turbulence-driven models in which the solar wind is powered by this flux.