MHD modeling of a geoeffective interplanetary CME with the magnetic topology informed by in-situ observations

TL;DR

This study develops a new MHD model to simulate the propagation of a specific geoeffective CME, incorporating observational data to accurately reproduce magnetic field variations at Earth.

Contribution

The paper introduces a novel numerical model that combines the Gibson-Low CME model with in-situ magnetic observations to better understand CME magnetic topology evolution.

Findings

Model successfully reproduces magnetic field rotation during CME passage.

Simulation results are consistent with in-situ magnetic field data for certain propagation directions.

The model confirms the East-West orientation of the CME flux rope.

Abstract

Variations of the magnetic field within solar coronal mass ejections (CMEs) in the heliosphere depend on the CME`s magnetic structure as it leaves the solar corona and its subsequent evolution through interplanetary space. To account for this evolution, we developed a new numerical model of the inner heliosphere that simulates the propagation of a CME through a realistic background solar wind and allows various CME magnetic topologies. To this end, we incorporate the Gibson-Low CME model within our global MHD model of the inner heliosphere, GAMERA-Helio. We apply the model to study the propagation of the geoeffective CME that erupted on 3 April, 2010 with the aim to reproduce the temporal variations of the magnetic field vector during the CME passage by Earth. Parameters of the Gibson-Low CME are informed by STEREO white-light observations near the Sun. The magnetic topology for this CME - the tethered flux rope - is informed by in-situ magnetic field observations near Earth. We performed two simulations testing different CME propagation directions. For an in-ecliptic direction, the simulation shows a rotation of all three magnetic field components within the CME, as seen at Earth, similar to that observed. With a southward propagation direction, suggested by coronal imaging observations, the modeled By and Bz components are consistent with the ACE data, but the Bx component lacks the observed change from negative to positive. In both cases, the model favors the East-West orientation of the CME flux rope, consistent with the orientation previously inferred from the STEREO/HI heliospheric images.