Evolution of CME Properties in the Inner Heliosphere: Prediction for Solar Orbiter and Parker Solar Probe

TL;DR

This study models the evolution of CME properties in the inner heliosphere using simulations with different initiation mechanisms, comparing results with existing observational data to enhance understanding of CME behavior near the Sun.

Contribution

It introduces simulated CME evolution in the inner heliosphere with two initiation mechanisms and compares these with observational data, filling the data gap below 0.29 au.

Findings

CME size and magnetic field strength evolution are similar for different flux rope models.

Simulation results align with previous observational and remote sensing studies.

The evolution patterns are consistent with statistical data from Helios and MESSENGER.

Abstract

The evolution of the magnetic field and plasma quantities inside a coronal mass ejection (CME) with distance are known from statistical studies using data from 1 au monitors, planetary missions, Helios, and Ulysses. This does not cover the innermost heliosphere, below 0.29 au, where no data are yet publicly available. Here, we describe the evolution of the properties of simulated CMEs in the inner heliosphere using two different initiation mechanisms. We compare the radial evolution of these properties with that found from statistical studies based on observations in the inner heliosphere by Helios and MESSENGER. We find that the evolution of the radial size and magnetic field strength is nearly indistinguishable for twisted flux rope from that of writhed CMEs. The evolution of these properties is also consistent with past studies, primarily with recent statistical studies using in situ measurements and with studies using remote observations of CMEs.