3D electron density distributions in the solar corona during solar minima: assessment for more realistic solar wind modeling

TL;DR

This study derives 4D electron density distributions in the solar corona during solar minima using a new tomographic method, compares results with models, and explores implications for solar wind origins and structure rotation.

Contribution

It introduces a novel time-dependent tomographic reconstruction technique for 4D electron density mapping in the solar corona during minima, improving accuracy over previous methods.

Findings

Thermodynamic models produce more realistic density values than polytropic models.

Tomography accurately captures polar regions and coronal structure evolution.

High-density structures often follow pseudo-streamers, not just the heliospheric current sheet.

Abstract

Knowledge of the electron density distribution in the solar corona put constraints on the magnetic field configurations for coronal modeling and on initial conditions for solar wind modeling. We work with polarized SOHO/LASCO-C2 images from the last two recent minima of solar activity (1996-1997 and 2008-2010), devoid of coronal mass ejections. The goals are to derive the 4D electron density distributions in the corona by applying a newly developed time-dependent tomographic reconstruction method and to compare the results between the two solar minima and with two magnetohydrodynamic models. First, we confirm that the values of the density distribution in thermodynamic models are more realistic than in polytropic ones. The tomography provides more accurate distributions in the polar regions, and we find that the density in tomographic and thermodynamic solutions varies with the solar cycle in both polar and equatorial regions. Second, we find that the highest-density structures do not always correspond to the predicted large-scale heliospheric current sheet or its helmet streamer but can follow the locations of pseudo-streamers. We deduce that tomography offers reliable density distributions in the corona, reproducing the slow time evolution of coronal structures, without prior knowledge of the coronal magnetic field over a full rotation. Finally, we suggest that the highest-density structures show a differential rotation well above the surface depending on how they are magnetically connected to the surface. Such valuable information on the rotation of large-scale structures could help to connect the sources of the solar wind to their in situ counterparts in future missions such as Solar Orbiter and Solar Probe Plus.