MHD Modeling of Solar Coronal Magnetic Evolution Driven by Photospheric Flow
It is well-known that magnetic fields dominate the dynamics in the solar corona, and new generation of numerical modeling of the evolution of coronal magnetic fields, as featured with boundary conditions driven directly by observation data, are being developed. This paper describes a new approach of...
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doaj-cd5a000ddc7c4f3994e0cd721cd1b8f42021-05-17T06:06:45ZengFrontiers Media S.A.Frontiers in Physics2296-424X2021-05-01910.3389/fphy.2021.646750646750MHD Modeling of Solar Coronal Magnetic Evolution Driven by Photospheric FlowChaowei JiangXinkai BianTingting SunXueshang FengIt is well-known that magnetic fields dominate the dynamics in the solar corona, and new generation of numerical modeling of the evolution of coronal magnetic fields, as featured with boundary conditions driven directly by observation data, are being developed. This paper describes a new approach of data-driven magnetohydrodynamic (MHD) simulation of solar active region (AR) magnetic field evolution, which is for the first time that a data-driven full-MHD model utilizes directly the photospheric velocity field from DAVE4VM. We constructed a well-established MHD equilibrium based on a single vector magnetogram by employing an MHD-relaxation approach with sufficiently small kinetic viscosity, and used this MHD equilibrium as the initial conditions for subsequent data-driven evolution. Then we derived the photospheric surface flows from a time series of observed magentograms based on the DAVE4VM method. The surface flows are finally inputted in time sequence to the bottom boundary of the MHD model to self-consistently update the magnetic field at every time step by solving directly the magnetic induction equation at the bottom boundary. We applied this data-driven model to study the magnetic field evolution of AR 12158 with SDO/HMI vector magnetograms. Our model reproduced a quasi-static stress of the field lines through mainly the rotational flow of the AR's leading sunspot, which makes the core field lines to form a coherent S shape consistent with the sigmoid structure as seen in the SDO/AIA images. The total magnetic energy obtained in the simulation matches closely the accumulated magnetic energy as calculated directly from the original vector magnetogram with the DAVE4VM derived flow field. Such a data-driven model will be used to study how the coronal field, as driven by the slow photospheric motions, reaches a unstable state and runs into eruptions.https://www.frontiersin.org/articles/10.3389/fphy.2021.646750/fullmagnetic fieldmagnetohydodynamicnumerical modelingsolar coronaphotospheric flow |
collection |
DOAJ |
language |
English |
format |
Article |
sources |
DOAJ |
author |
Chaowei Jiang Xinkai Bian Tingting Sun Xueshang Feng |
spellingShingle |
Chaowei Jiang Xinkai Bian Tingting Sun Xueshang Feng MHD Modeling of Solar Coronal Magnetic Evolution Driven by Photospheric Flow Frontiers in Physics magnetic field magnetohydodynamic numerical modeling solar corona photospheric flow |
author_facet |
Chaowei Jiang Xinkai Bian Tingting Sun Xueshang Feng |
author_sort |
Chaowei Jiang |
title |
MHD Modeling of Solar Coronal Magnetic Evolution Driven by Photospheric Flow |
title_short |
MHD Modeling of Solar Coronal Magnetic Evolution Driven by Photospheric Flow |
title_full |
MHD Modeling of Solar Coronal Magnetic Evolution Driven by Photospheric Flow |
title_fullStr |
MHD Modeling of Solar Coronal Magnetic Evolution Driven by Photospheric Flow |
title_full_unstemmed |
MHD Modeling of Solar Coronal Magnetic Evolution Driven by Photospheric Flow |
title_sort |
mhd modeling of solar coronal magnetic evolution driven by photospheric flow |
publisher |
Frontiers Media S.A. |
series |
Frontiers in Physics |
issn |
2296-424X |
publishDate |
2021-05-01 |
description |
It is well-known that magnetic fields dominate the dynamics in the solar corona, and new generation of numerical modeling of the evolution of coronal magnetic fields, as featured with boundary conditions driven directly by observation data, are being developed. This paper describes a new approach of data-driven magnetohydrodynamic (MHD) simulation of solar active region (AR) magnetic field evolution, which is for the first time that a data-driven full-MHD model utilizes directly the photospheric velocity field from DAVE4VM. We constructed a well-established MHD equilibrium based on a single vector magnetogram by employing an MHD-relaxation approach with sufficiently small kinetic viscosity, and used this MHD equilibrium as the initial conditions for subsequent data-driven evolution. Then we derived the photospheric surface flows from a time series of observed magentograms based on the DAVE4VM method. The surface flows are finally inputted in time sequence to the bottom boundary of the MHD model to self-consistently update the magnetic field at every time step by solving directly the magnetic induction equation at the bottom boundary. We applied this data-driven model to study the magnetic field evolution of AR 12158 with SDO/HMI vector magnetograms. Our model reproduced a quasi-static stress of the field lines through mainly the rotational flow of the AR's leading sunspot, which makes the core field lines to form a coherent S shape consistent with the sigmoid structure as seen in the SDO/AIA images. The total magnetic energy obtained in the simulation matches closely the accumulated magnetic energy as calculated directly from the original vector magnetogram with the DAVE4VM derived flow field. Such a data-driven model will be used to study how the coronal field, as driven by the slow photospheric motions, reaches a unstable state and runs into eruptions. |
topic |
magnetic field magnetohydodynamic numerical modeling solar corona photospheric flow |
url |
https://www.frontiersin.org/articles/10.3389/fphy.2021.646750/full |
work_keys_str_mv |
AT chaoweijiang mhdmodelingofsolarcoronalmagneticevolutiondrivenbyphotosphericflow AT xinkaibian mhdmodelingofsolarcoronalmagneticevolutiondrivenbyphotosphericflow AT tingtingsun mhdmodelingofsolarcoronalmagneticevolutiondrivenbyphotosphericflow AT xueshangfeng mhdmodelingofsolarcoronalmagneticevolutiondrivenbyphotosphericflow |
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1721438674800869376 |