Magnetohydrodynamic simulation of the 2012-July-12 CME Event With the Fluxrope-G3DMHD Model

TL;DR

This paper presents a new magnetohydrodynamic model combining a data-driven approach and a magnetic flux-rope model to simulate and predict the evolution of a significant CME event from the Sun to Earth.

Contribution

The paper introduces a novel integrated MHD model that accurately simulates CME evolution and magnetic field profiles, improving space weather prediction capabilities.

Findings

Successfully reproduces shock, sheath, and flux rope features observed by Wind spacecraft.

Accurately simulates the evolution of the 2012 CME event from Sun to Earth.

Provides a promising tool for space weather forecasting.

Abstract

Coronal mass ejections (CMEs) and their driven shocks are a major source of large geomagnetic storms due to their large and long-lasting, southward component of magnetic field in the sheath and the flux rope (e.g., magnetic cloud). Predicting the strength and arrival time of southward fields accurately thus plays a key role in space weather predictions. To address this problem, we have developed a new model, which combines the global three-dimensional, time-dependent, magnetohydrodynamic (MHD), data-driven model (G3DMHD) and a self-contained magnetic flux-rope model [1]. As a demonstration and validation, here we simulate the evolution of a Sun-Earth-directed CME that erupted on 2012-July-12. The computational domain spans from 2.5 solar radii (Rs) from the surface of the Sun, where the flux rope is injected, to 245 Rs. We compare the time profiles of the simulated MHD parameters (Density, velocity, temperature, and magnetic field) with in situ solar wind observations acquired at ~1 AU by the Wind spacecraft and the result is encouraging. The model successfully reproduces the shock, sheath, and flux rope similar to those observed by Wind.