Tetsuya Magara

TL;DR: The current understanding of solar flares, mainly focused on magnetohydrodynamic (MHD) processes responsible for producing a flare, can be found in this article, where the authors present a review of the models proposed to explain the physical mechanism of flares, giving an comprehensive explanation of the key processes.

TL;DR: In this paper, a detailed kinematic measurement of the small-scale turbulent upflows seen in several prominences in the SOT database is presented, and the authors conclude that buoyant plumes are a source of quiescent prominence mass as well as a mechanism by which prominence plasma is advected upward.

TL;DR: In this article, the authors investigated the twist and connectivity of magnetic field lines in the flare-productive active region NOAA 10930 in terms of the vector magnetograms observed by the Solar Optical Telescope on board the Hinode satellite and the nonlinear force-free field (NLFFF) extrapolation.

TL;DR: In this article, the authors discuss the role of the sigmoid eruption in triggering the flare, which consists of two different sets of ribbons: parallel ribbons and a large-scale quasi-circular ribbon.

TL;DR: In this paper, the temporal evolution of the three-dimensional magnetic structure of the flaring active region (AR) NOAA 10930 was analyzed by using the nonlinear force-free fields extrapolated from the photospheric vector magnetic fields observed by the Solar Optical Telescope on board Hinode.