Magnetic field extrapolation in active region well comparable with observations in multiple layers
arXiv:2210.15074 · doi:10.3847/1538-4357/acd112
Abstract
Magnetic field extrapolation is a fundamental tool to reconstruct the three-dimensional magnetic field above the solar photosphere. However, the prevalently used force-free field model might not be applicable in the lower atmosphere with non-negligible plasma \b{eta}, where the crucial process of flux rope formation and evolution could happen. In this work, we perform extrapolation in active region (AR) 12158, based on an recently developed magnetohydrostatic (MHS) method which takes plasma forces into account. By comparing the results with those from the force-free field extrapolation methods, we find that the overall properties, which are characterized by the magnetic free energy and helicity, are roughly the same. The major differences lie in the magnetic configuration and the twist number of magnetic flux rope (MFR). Unlike previous works either obtained sheared arcades or one coherent flux rope, the MHS method derives two sets of MFR, which are highly twisted and slightly coupled. Specifically, the result in the present work is more comparable with the high-resolution observations from the chromosphere, through the transition region to the corona, such as the filament fibrils, pre-eruptive braiding characteristics and the eruptive double-J shaped hot channel. Overall, our work shows that the newly developed MHS method is more promising to reproduce the magnetic fine structures that can well match the observations at multiple layers, and future data-driven simulation based on such extrapolation will benefit in understanding the critical and precise dynamics of flux rope before eruption.
The paper titled with 'Does the non-force-freeness matter for the extrapolation of solar magnetic field?' has been withdrawn, it is now replaced with a new paper titled with 'Magnetic field extrapolation in active region well comparable with observations in multiple layers'
References in corpus (31)
- Torus instability
- The Helioseismic and Magnetic Imager (HMI) Vector Magnetic Field Pipeline: SHARPs -- Space-weather HMI Active Region Patches
- The Helioseismic and Magnetic Imager (HMI) Vector Magnetic Field Pipeline: Overview and Performance
- Ideal kink instability of a magnetic loop equilibrium
- Optimization code with weighting function for the reconstruction of coronal magnetic fields
- Observation of An Evolving Magnetic Flux Rope Prior To and During A Solar Eruption
- The solar magnetic field
- Nonlinear force-free modeling of the solar coronal magnetic field
- A fundamental mechanism of solar eruption initiation
- Formation of a Double-decker Magnetic Flux Rope in the Sigmoidal Solar Active Region 11520
- Structures of Interplanetary Magnetic Flux Ropes and Comparison with Their Solar Sources
- On fibrils and field lines: The nature of H fibrils in the solar chromosphere
- Magnetic helicity estimations in models and observations of the solar magnetic field. Part I: Finite volume methods
- On the twists of interplanetary magnetic flux ropes observed at 1 AU
- Imaging and Spectroscopic Diagnostics on the Formation of Two Magnetic Flux Ropes Revealed by SDO/AIA and IRIS
- Can We Improve the Preprocessing of Photospheric Vector Magnetograms by the Inclusion of Chromospheric Observations?
- The role of non-axisymmetry of magnetic flux rope in constraining solar eruptions
- Magnetic helicity budget of solar active regions prolific of eruptive and confined flares
- Temporal Evolution of the Magnetic Topology of the NOAA Active Region 11158
- Magnetic helicity and energy budget around large confined and eruptive solar flares
- Links between magnetic fields and plasma flows in a coronal hole
- Sunspot Rotation as a Driver of Major Solar Eruptions in NOAA Active Region 12158
- Observational Evidence of Magnetic Reconnection for Brightenings and Transition Region Arcades in IRIS observations
- Initiation and Eruption Process of Magnetic Flux Rope from Solar Active Region NOAA 11719 to Earth Directed-CME
- FastQSL: A Fast Computation Method for Quasi-separatrix Layers
- Magnetic Twists of Solar Filaments
- Comparison of Two Coronal Magnetic Field Models for Reconstructing a Sigmoidal Solar Active Region With Coronal Loops
- Test magnetohydrostatic extrapolation with radiative MHD simulation of a solar flare
- Relative magnetic field line helicity
- Helical Twisting Number and Braiding Linkage Number of Solar Coronal Loops
- Magnetohydrostatic modeling of AR11768 based on a SUNRISE/IMaX vector magnetogram