SHINE: Using Two-Ribbon Flare Observations and Magnetohydrodynamics (MHD) Simulations to Study Eruptive Flares and Their Relationship to Coronal Mass Ejections (CMEs)

University Of California-Berkeley, Berkeley CA

Investigators

Abstract

Two-ribbon flares are the most powerful and potentially geoeffective type of solar flares. This 3-year SHINE project aims to investigate the dynamics of solar flare ribbons, and relate them to photospheric magnetic structures and properties of Coronal Mass Ejections (CMEs). The team will develop an ensemble database of the two-ribbon flares in combination with magnetohydrodynamic (MHD) simulations of CMEs to understand the relation between reconnection flux and CME properties. The project addresses the question of how flare ribbons develop, and how they are associated with CMEs, which is very important for understanding the fundamental physics of solar eruptions. The ability to relate large-scale CME properties to the source-region flare properties based on a much larger dataset and supported by theoretical MHD context will allow for improved space weather forecasts (e.g., more accurate CME arrival times at 1 AU) and methods, addressing the main goal of the SHINE community and the ability to protect our assets in Space. The scientific outcome of this project will enhance scientific and technological understanding of solar flares, enabling readiness for the Daniel K. Inouye Solar Telescope (DKIST) and application of more realistic and computationally sophisticated data-driven MHD models. The research project will be led by junior female scientist at UC Berkeley who will work with several undergraduate students at the host institution. The research and EPO agenda of this project supports the Strategic Goals of the AGS Division in discovery, learning, diversity, and interdisciplinary research. This SHINE project aims to utilize the newly assembled database of flare-ribbon maps (within 45 degrees of disk center) and reconnection fluxes of all two-ribbon flares (C1.0 and above) observed during the Solar Dynamics Observatory (SDO) era to investigate how ribbons properties are related to other flare and CME properties, both from the observational and modeling points of view. For all events, the project team will calculate vector magnetic field inclination, shear and the vertical electric current evolution inside and outside flare ribbons. Where CME observations permit, the team will quantify the relationship between large-scale CME properties, including the CME speed, acceleration and the magnetic flux from the in-situ observed interplanetary CME (ICME) and compare those with the ribbon's properties above. For three distinct events of solar eruptions associated with slow, moderate and fast CMEs, the investigators will perform 3D MHD simulations and analyze their flare ribbons and CME/ICME properties to provide the theoretical context and guidance to fully understand the observations.