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Research Topics
My research field is solar plasma physics focusing on explosive phenomena in the solar corona.
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.Fundermental MHD processes, magnetic reconnection, MHD instability in the solar flares.
iv. 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
The coronal magnetic field is the source of energetic phenomena observed in the solar corona, such as solar flares and coronal mass ejections (CMEs). To understand these dynamic events, it is essentual to investigate the three-dimensional (3D) magnetic field in the solar corona. However, direct measurements of the 3D coronal magnetic field are not possible; we can only observe the magnetic field at the photosphere. Therefore, extrapolation techniques
based on photospheric magnetic field observations are required to infer the coronal magnetic structure.
The upper figure on the right shows a reconstructed magnetic field under the force-free field approximation, which successfully reveals strongly sheared magnetic field lines. This structure is often referred to as a "sigmoid" and is widely considered to be a source of solar eruptions.
We are further developing new extrapolation methods to reconstruct force-free and magnetohydrostatic fields, enabling detailed analysis of the 3D coronal magnetic field and its role in solar dynamics.
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. Nonlinear Evolution of Torus Plasma
The evolution of torus plasma is an important research topic in both fusion plasma physics and solar astrophysics. In particular, its nonlinear evolution is essential for understanding confined plasmas in laboratory experiments and eruptive plasmas in the solar atmosphere. We investigate the evolution of line-tied semi-torus plasma configurations, which are relevant to the solar atmosphere. Under what conditions does magnetized torus plasma lead to eruptions or failed eruptions? This question is important not only for understanding the nonlinear dynamics of torus plasma, but also for improving the prediction of solar eruptions.
Evolution of magnetized semi-torus plasma obtained from an MHD simulation.
iv. Solar Flares and CME Triggering Process
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 Inoue, submitted, 2026.
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