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

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.

arXiv commentAccepted to APJ. * pages, 6 figures

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Cited by in corpus (6)

• Prediction of the in situ coronal mass ejection rate for solar cycle 25: Implications for Parker Solar Probe in situ observations
• Inconsistencies Between Local and Global Measures of CME Radial Expansion as Revealed by Spacecraft Conjunctions
• Evolution of a Long-Duration Coronal Mass Ejection and its Sheath Region Between Mercury and Earth on 2013 July 9-14
• Exploring the radial evolution of Interplanetary Coronal Mass Ejections using EUHFORIA
• On the utility of flux rope models for CME magnetic structure below 30$R_{\odot }$
• Modeling CME encounters at Parker Solar Probe with OSPREI: Dependence on photospheric and coronal conditions