Synthetic Remote-sensing and In-situ Observations of Fine-scale Structure in a Pseudostreamer Coronal Mass Ejection through the Solar Corona

TL;DR

This study uses synthetic remote-sensing and in-situ observations from simulations to analyze the fine-scale structure of a pseudostreamer-associated CME, aiding interpretation of Parker Solar Probe data.

Contribution

It introduces a detailed simulation framework producing synthetic observations of CME structures, enhancing understanding of pseudostreamer CMEs and their signatures.

Findings

Synthetic WISPR imagery reveals fine-scale CME structures.

Differences in plasma and field signatures depend on trajectory.

Simulation results inform interpretation of Parker Solar Probe data.

Abstract

Coronal pseudostreamer flux systems have a specific magnetic configuration that influences the morphology and evolution of coronal mass ejections (CMEs) from these regions. Here we continue the analysis of the Wyper et al. (2024, ApJ 975, 168) magnetohydrodynamic simulation of a CME eruption from an idealized pseudostreamer configuration through the construction of synthetic remote-sensing and in-situ observational signatures. We examine the pre-eruption and eruption signatures in extreme ultraviolet and white-light from the low corona through the extended solar atmosphere. We calculate synthetic observations corresponding to several Parker Solar Probe-like trajectories at $\sim$10$R_\odot$ to highlight the fine-scale structure of the CME eruption in synthetic WISPR imagery and the differences between the in-situ plasma and field signatures of flank and central CME-encounter trajectories. Finally, we conclude with a discussion of several aspects of our simulation results in the context of interpretation and analysis of current and future Parker Solar Probe data.