How coronal mass ejections are influenced by the morphology and toroidal flux of their source magnetic flux ropes?

• DOI: 10.48550/arxiv.2407.09457
• Publication Date: 2024-01-01
• Authors: Guo, J.H.; Linan, L.; Poedts, Stefaan; Guo, Y.; Schmieder, B.; Lani, A.; Ni, Y.W.; Brchnelova, M.; Perri, B.; Baratashvili, T.; Li, S.T.; Chen, P.F.
• Keywords: C14/19/089#55221731; Astrophysics - Solar and Stellar Astrophysics; Physics - Space Physics; G0B5823N#57353107; Astrophysics of Galaxies (astro-ph.GA); G002523N#57356925; FOS: Physical sciences; Astrophysics - Astrophysics of Galaxies; Solar and Stellar Astrophysics (astro-ph.SR); Space Physics (physics.space-ph)

driving significant changes of the heliospheric environment. Deducing the properties of CMEs from their progenitors in solar source regions is crucial for space weather forecasting. Aims. The primary objective of this paper is to establish a connection between CMEs and their progenitors in solar source regions, enabling us to infer the magnetic structures of CMEs before their full development. Methods. We create a dataset comprising a magnetic flux rope series with varying projection shapes (S-, Z- and toroid-shaped), sizes and toroidal fluxes, using the Regularized Biot-Savart Laws (RBSL). These flux ropes are inserted into solar quiet regions, aimed at imitating the eruptions of quiescent filaments. Thereafter, we simulate the propagation of these flux ropes from the solar surface to a distance of 25R⊙ with our global coronal magnetohydrodynamic (MHD) model which is named COCONUT. Results. Our parametric survey reveals significant impacts of source flux ropes on the consequent CMEs. Regarding the flux-rope morphology, we find that the projection shape (e.g., sigmoid or torus) can influence the magnetic structures of CMEs at 20R⊙, albeit with minimal impacts on the propagation speed. However, these impacts diminish as source flux ropes become fat. In terms of toroidal flux, our simulation results demonstrate a pronounced correlation with the propagation speed of CMEs, as well as the successfulness in erupting. Conclusions. This work builds the bridge between the CMEs in the outer corona and their progenitors in solar source regions. Our parametric survey suggests that the projection shape, cross-section radius and toroidal flux of source flux ropes are crucial parameters in predicting magnetic structures and propagation speed of CMEs, providing valuable insights for space weather prediction. On the one hand, the conclusion drawn here could be instructive in identifying the high-risk eruptions with the potential to induce stronger geomagnetic effects (Bz and propagation speed). On the other hand, our findings hold practical significance for refining the parameter settings of launched CMEs at 21.5R⊙ in heliospheric simulations, such as with EUHFORIA, based on observations for their progenitors in solar source regions.<br/>status: published<br/>ispartof: Astronomy & Astrophysics vol:690<br/>