On the Acceleration of the Young Solar Wind from Different Source Regions

TL;DR

This study analyzes the acceleration mechanisms of the young solar wind from different source regions using Parker Solar Probe data, highlighting the roles of proton and electron pressures and the potential influence of Alfvén waves.

Contribution

It provides the first statistical analysis of solar wind acceleration from various source regions and demonstrates the importance of proton pressure differences in wind speed variations.

Findings

Proton pressure differences drive wind speed variations.

Proton temperature correlates quadratically with wind speed.

Alfvén waves may contribute to wind acceleration, especially in fast winds.

Abstract

The acceleration of the young solar wind is studied using the first 17 encounters of Parker Solar Probe. We identify wind intervals from different source regions: coronal hole (CH) interiors, streamers, and low Mach number boundary layers (LMBLs), i.e. the inner boundaries of coronal holes. We present their statistical trends in the acceleration process. Most of the observations can be reproduced by a two-fluid hydrodynamic model with realistic corona temperatures. In such a model, the solar wind is accelerated by the combined thermal pressures of protons and electrons,but it is mainly the difference in the proton pressure that leads to the difference in the solar wind speed. The proton pressure is the highest in the fastest CH wind, with a high initial proton temperature that decreases slowly. It is lower in the relatively slow LMBL wind, and the lowest in the slowest streamer wind. The proton temperature is quadratically correlated with the wind speed when scaled to the same distance. In contrast, the electron temperature shows no significant differences for different wind types or wind speeds, indicating more similar contributions from the electron pressure. The model gives reasonable locations for the sonic critical point, which is on average at 3.6-7.3 solar radii and can also extend to large distances when the proton temperature is extremely low, as in the LMBL wind. In addition to the thermal pressure, we raise the possibility that Alfv\'en waves may contribute to the solar wind acceleration, especially for the fast CH wind.