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79 papers
Thermodynamic properties of small flares in the quiet Sun observed by H and EUV: plasma motion of the chromosphere and time evolution of temperature/emission measure
Yuji Kotani, Takako T. Ishii, Daiki Yamasaki +4
Small flares frequently occur in the quiet Sun. Previous studies have noted that they share many common characteristics with typical solar flares in active regions. However, their…
Magnetic Field of Solar Dark Filaments Obtained from He I 10830 Angstrom Spectro-polarimetric Observation
Daiki Yamasaki, Yu Wei Huang, Yuki Hashimoto +4
Solar filaments are dense and cool plasma clouds in the solar corona. They are supposed to be supported in a dip of coronal magnetic field. However, the models are still under argu…
Unified Relationship between Cold Plasma Ejections and Flare Energies Ranging from Solar Microflares to Giant Stellar Flares
Yuji Kotani, Kazunari Shibata, Takako T. Ishii +4
We often find spectral signatures of chromospheric cold plasma ejections accompanied by flares in a wide range of spatial scales in the solar and stellar atmospheres. However, the…
Sun-as-a-star Analyses of Various Solar Active Events Using H Spectral Images Taken by SMART/SDDI
Takato Otsu, Ayumi Asai, Kiyoshi Ichimoto +2
Sun-as-a-star analyses, in which observational data is spatially integrated, are useful for interpreting stellar data. For future applications to stellar observations, we performed…
Polarization calibration of the Tandem Etalon Magnetograph of the Solar Magnetic Activity Research Telescope at Hida Observatory
Daiki Yamasaki, Shin'ichi Nagata, Kiyoshi Ichimoto
The Tandem Etalon Magnetograph (TEM) is one of the instruments of the Solar Magnetic Activity Research Telescope of Hida Observatory. The TEM is a partial disk (320" x240") filter…
Sun-as-a-star Analysis of H Spectra of a Solar Flare Observed by SMART/SDDI: Time Evolution of Red Asymmetry and Line Broadening
Kosuke Namekata, Kiyoshi Ichimoto, Takako T. Ishii +1
Stellar flares sometimes show red/blue asymmetries of H line, which can indicate chromospheric dynamics and prominence activations. However, the origin of asymmetries is not com…