Estimating the Magnetic Structure of an Erupting CME Flux Rope From AR12158 Using Data-Driven Modeling

Frontiers in Astronomy and Space Sciences

Daniel Price¹  Ranadeep Sarkar¹  Jens Pomoell¹  Eleanna Asvestari¹  Emilia K. J. Kilpua² 

[1] Department of Physics, University of Helsinki, Helsinki, Finland;null;

关键词: magnetic fields;    solar wind;    corona;    coronal mass ejection;    flux ropes;    space weather;   

DOI  :  10.3389/fspas.2021.631582

来源: Frontiers

【 摘 要 】

We investigate here the magnetic properties of a large-scale magnetic flux rope related to a coronal mass ejection (CME) that erupted from the Sun on September 12, 2014 and produced a well-defined flux rope in interplanetary space on September 14–15, 2014. We apply a fully data-driven and time-dependent magnetofrictional method (TMFM) using Solar Dynamics Observatory (SDO) magnetograms as the lower boundary condition. The simulation self-consistently produces a coherent flux rope and its ejection from the simulation domain. This paper describes the identification of the flux rope from the simulation data and defining its key parameters (e.g., twist and magnetic flux). We define the axial magnetic flux of the flux rope and the magnetic field time series from at the apex and at different distances from the apex of the flux rope. Our analysis shows that TMFM yields axial magnetic flux values that are in agreement with several observational proxies. The extracted magnetic field time series do not match well with in-situ components in direct comparison presumably due to interplanetary evolution and northward propagation of the CME. The study emphasizes also that magnetic field time-series are strongly dependent on how the flux rope is intercepted which presents a challenge for space weather forecasting.

【 授权许可】

CC BY