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Research Topics
My research field is solar plasma physics, now focusing on....
i. MHD modeling of magnetic fields in solar active region and solar corona
ii. MHD modeling of the solar storm: eruptions, flares, CMEs, formation and dynamics of solar flux rope.
iii.Nonlinear MHD process, the magnetic reconnection, MHD instability in the solar corona.
iv. in futuer... particle acceleration in the solar flare
v. in future...flare CME prediction to contribute to space weather.
i. Data-Based Modeling of Solar Magnetic Fields
Coronal magnetic field is a source of energetic phenomena observed in the solar corona, such as solar flares and coronal mass ejections (CMEs). In order to clarify these dynamics , it is important to understand the three-dimensional (3D) magnetic structure in the solar corona. But, unfortunately, we cannot directly measure the 3D coronal magnetic field, rather only on the photosphere. We thus need the extrapolation based on the observed photospheric magnetic field to extract the information of the 3D magnetic fields. The right figure shows the reconstructed fields under the force-free approximation that can successfully show the strong sheared fields. These field lines stucture are often called as 'Sigmoid' and widely accepted as a source of the solar eruptions. We further develop new extrapolation method to achieve the force-free field or magnetohydro-static field, and analyze the 3D magnetic field to understand the dynamics of the coronal magnetic field.
Nonlinear Force-Free Field of AR12017 from Inoue PEPS, 2016
ii.Data-Based/Inspired MHD Simulation of Solar Eruptions
Solar eruptions are widely considered as cause of the space storm in our Geospace. These phenomena are interesting too for a nonlinear dynamics of the solar plasma, not only for the space weather forecasts. In order to understand the dynamics of the solar eruptions covering from the triggering process to CME formation, we conduct the research in term of the magnetohydrodynamic simulations. Recently, we conduct the simulations combined with the observation, which are often called as data-constrained or data-driven simulation. We further develop new simulation techniques to consistently interact with observed data as well as clarify the basic physics of solar eruptions.
Solar Eruption from AR11158.
Inoue + Nature Communications 2018
Formation of erupting flux rope
in AR12371.
Erupting flux rope in AR12673.
Inoue et al. 2018, ApJ
Summary of Flare-CME relationship propsed by Inoue et al. PEPS 2016
iii.MHD Phenomena in the Sun and Astrophysical Phenomena
We usually encounter the complex nonlinear dynamics in solar eruptions and in other solar MHD phenomena. We are trying to figure out these nonlinear processes using a numerical simulation. The right figure shows one of the results where the initial sheared field lines are broken due to interact with a small-scale emerging flux, resulting in ejective eruption. We found the two kind of the eruptions: one is instability-driven eruption and another one is reconnection-driven eruption with different magnitude of the small-scale emerging flux.
This result suggest a possibiltiy of two initiation mechanism under even same initial sate.
An MHD simulation of the solar eruption triggered by a small-scale emerging flux, From Nguyen & Inoue, in preparation 2024.
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