Multi spacecraft study with the Icarus model: Modelling the propagation of CMEs to Mercury and Earth

TL;DR

This study evaluates the Icarus heliospheric model's ability to simulate CME propagation to Mercury and Earth, demonstrating its effectiveness and limitations through comparison with in-situ spacecraft measurements.

Contribution

The paper introduces and validates the Icarus model for CME propagation, incorporating adaptive mesh refinement and multi-spacecraft data for improved space weather prediction accuracy.

Findings

Model accurately reproduces CME profiles at Mercury and Earth

Higher AMR levels improve small-scale feature resolution

Complex CME interactions require modeling multiple events

Abstract

Coronal Mass Ejections (CMEs) are the main drivers of the disturbances in interplanetary space. Understanding the CME interior magnetic structure is crucial for advancing space weather studies. Assessing the capabilities of a numerical heliospheric model is crucial, as understanding the nature and extent of its limitations can be used for improving the model and the space weather predictions based on it. The present paper aims to test the capabilities of the recently developed heliospheric model Icarus and the linear force-free spheromak model that has been implemented in it. To validate the Icarus space weather modeling tool, two CME events were selected that were observed by two spacecraft located near Mercury and Earth, respectively. This enables testing the heliospheric model computed with Icarus at two distant locations. The source regions for the CMEs were identified, and the CME parameters were determined and later optimized. Different adaptive mesh refinement levels were applied in the simulations to assess its performance by comparing the simulation results to in-situ measurements. The first CME event erupted on SOL2013-07-09T15:24. The modeled time series were in good agreement with the observations both at MESSENGER and ACE. The second CME event started on SOL2014-02-16T10:24 and was more complicated, as three CME interactions occurred in this event. It was impossible to recover the observed profiles without modeling the other two CMEs that were observed, one before the main CME and one afterward. For both CME studies, AMR level 3 was sufficient to reconstruct small-scale features near Mercury, while at Earth, AMR level 4 was necessary due to the radially stretched grid that was used.