Thermodynamic and Magnetic Topology Evolution of the X1.0 Flare on 2021 October 28 Simulated by a Data-driven Radiative Magnetohydrodynamic Model

Abstract

Solar filament eruptions, flares, and coronal mass ejections (CMEs) are manifestations of drastic releases of energy in the magnetic field, which are related to many eruptive phenomena, from the Earth’s magnetosphere to black hole accretion disks. With the availability of high-resolution magnetograms on the solar surface, observational data-based modeling is a promising way to quantitatively study the underlying physical mechanisms behind observations. By incorporating thermal conduction and radiation losses in the energy equation, we develop a new data-driven radiative magnetohydrodynamic model, which has the capability of capturing the thermodynamic evolution compared to our previous zero-β model. Our numerical results reproduce the major observational characteristics of the X1.0 flare on 2021 October 28 in NOAA active region 12887, including the morphology of the eruption, the kinematics of the flare ribbons, extreme ultraviolet (EUV) radiations, and the two components of the EUV waves predicted by the magnetic stretching model, i.e., a fast-mode shock wave and a slower apparent wave, due to successive stretching of the magnetic field lines. Moreover, some intriguing phenomena are revealed in the simulation. We find that flare ribbons separate initially and ultimately stop at the outer stationary quasi-separatrix layers (QSLs). Such outer QSLs correspond to the border of the filament channel and determine the final positions of flare ribbons, which can be used to predict the size and the lifetime of a flare before it occurs. In addition, the side views of the synthesized EUV and white-light images exhibit typical three-part structures of CMEs, where the bright leading front is roughly cospatial with the nonwave component of the EUV wave, reinforcing the use of the magnetic stretching model for the slow component of EUV waves.

First Detection of Transverse Vertical Oscillation during the Expansion of Coronal Loops

“…In the future, in-depth investigations of the interaction between EUV waves and coronal loops are highly desirable, especially using high-resolution observations from the Extreme Ultraviolet Imager (EUI; Rochus et al 2020) on board Solar Orbiter (SO; Müller et al 2020). State-of-the-art MHD numerical simulations are greatly expected to explain the loop dynamics (Downs et al 2021;Wang et al 2021;Guo et al 2023).…”

Understanding the Lateral Drifting of an Erupting Filament with a Data-constrained Magnetohydrodynamic Simulation

“…In this process, some sheared arcades are converted into a part of the flux rope (orange lines). To see the radiative features of this eruption process, we also synthesize the optically thin radiation images at 171 and 335 Å wave bands, as done in Guo et al (2023). First, we calculate the emission in each cell with the following formula:…”

“…Additionally, the strong magnetic field in simulations is prone to lead to issues such as magnetic-field divergence and the occurrence of the "negative pressure" problem. Therefore, to speed up the computation and reduce numerical dissipation, the magnetic field is modified to one-tenth of the original observed data (see also Jiang et al 2016;Kaneko et al 2021;Guo et al 2023). Even so, the evolution of key magnetic structures during the eruption can be captured.…”

“…Such models have played a tremendous role in reproducing the 3D evolution of the magnetic fields (Cheung & DeRosa 2012;Jiang et al 2016;Inoue et al 2018aInoue et al , 2018bGuo et al 2019;Y. Guo et al 2021;Pomoell et al 2019) and the thermodynamics (Török et al 2018;Fan 2022;Guo et al 2023) in the corona, as well as the ICME propagation in the interplanetary space (Pomoell & Poedts 2018;Poedts et al 2020;Scolini et al 2020;Verbeke et al 2022). Here, we perform a nonadiabatic data-constrained magnetohydrodynamic (MHD) simulation of the filament eruption event that occurred on 2022 August 18, which exhibits obvious lateral drifting during its ascent, as captured by Solar Dynamics Observatory (SDO; Pesnell et al 2012) and Chinese Hα Solar Explorer (CHASE; Li et al 2019Li et al , 2022 simultaneously.…”

Transverse Vertical Oscillations During the Contraction and Expansion of Coronal Loops

“…In the future, in-depth investigations of the interaction between EUV waves and coronal loops are highly desirable, especially using high-resolution observations from the Extreme Ultraviolet Imager (Rochus et al 2020) on board Solar Orbiter (Müller et al 2020). State-of-the-art MHD numerical simulations are greatly expected to explain the loop dynamics (Downs et al 2021;Wang et al 2021;Guo et al 2023).…”