# Simulating Solar Coronal Mass Ejections constrained by Observations of their Speed and Poloidal flux

## TL;DR

This paper presents a method to constrain CME parameters using remote observations and simulations, achieving accurate modeling of CME speed and poloidal flux by integrating observational data with the MS-FLUKSS simulation suite.

## Contribution

The study introduces a data-driven approach to constrain CME model parameters using remote observations, improving simulation accuracy of CME speed and magnetic flux.

## Key findings

- Simulated CME speed of 840 km/s closely matches observed 812 km/s.
- Estimated poloidal flux of 5.1e21 Mx aligns with observational estimate of 4.9e21 Mx.
- Demonstrated approach effectively models CME propagation in a realistic solar corona background.

## Abstract

We demonstrate how the parameters of a Gibson-Low flux-rope-based coronal mass ejection (CME) can be constrained using remote observations. Our Multi Scale Fluid-Kinetic Simulation Suite (MS-FLUKSS) has been used to simulate the propagation of a CME in a data driven solar corona background computed using the photospheric magnetogram data. We constrain the CME model parameters using the observations of such key CME properties as its speed, orientation, and poloidal flux. The speed and orientation are estimated using multi-viewpoint white-light coronagraph images. The reconnected magnetic flux in the area covered by the post eruption arcade is used to estimate the poloidal flux in the CME flux rope. We simulate the partial halo CME on 7 March 2011 to demonstrate the efficiency of our approach. This CME erupted with the speed of 812 km/s and its poloidal flux, as estimated from source active region data, was 4.9e21 Mx. Using our approach, we were able to simulate this CME with the speed 840 km/s and the poloidal flux of 5.1e21 Mx, in remarkable agreement with the observations.