Zobrazeno 1 - 10
of 472
pro vyhledávání: '"ICHIMOTO, Kiyoshi"'
Autor:
Anan, Tetsu, Casini, Roberto, Uitenbroek, Han, Schad, Thomas A., Socas-Navarro, Hector, Ichimoto, Kiyoshi, Jaeggli, Sarah A., Tiwari, Sanjiv K., Reep, Jeffrey W., Katsukawa, Yukio, Asai, Ayumi, Qiu, Jiong, Reardon, Kevin P., Tritschler, Alexandra, Wöger, Friedrich, Rimmele, Thomas R.
The efficient release of magnetic energy in astrophysical plasmas, such as during solar flares, can in principle be achieved through magnetic diffusion, at a rate determined by the associated electric field. However, attempts at measuring electric fi
Externí odkaz:
http://arxiv.org/abs/2410.09221
A fast-filament eruption observed in the H$\alpha$ spectral line. I. Imaging spectroscopy diagnostic
Autor:
Cabezas, Denis P., Ichimoto, Kiyoshi, Asai, Ayumi, UeNo, Satoru, Morita, Satoshi, Otsuji, Ken-ichi, Shibata, Kazunari
Context. Solar filament eruptions usually appear to occur in association with the sudden explosive release of magnetic energy accumulated in long-lived arched magnetic structures. It is the released energy that occasionally drives fast-filament erupt
Externí odkaz:
http://arxiv.org/abs/2406.20020
Autor:
Kotani, Yuji, Ishii, Takako T., Yamasaki, Daiki, Otsuji, Kenichi, Ichimoto, Kiyoshi, Asai, Ayumi, Shibata, Kazunari
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 similarities and differences are not fully understood, especially thei
Externí odkaz:
http://arxiv.org/abs/2304.12037
Autor:
Yamasaki, Daiki, Huang, Yu Wei, Hashimoto, Yuki, Cabezas, Denis P., Kawate, Tomoko, UeNo, Satoru, Ichimoto, Kiyoshi
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 argument between two types of the field configuration; one is the normal p
Externí odkaz:
http://arxiv.org/abs/2304.00422
Autor:
Kotani, Yuji, Shibata, Kazunari, Ishii, Takako T., Yamasaki, Daiki, Otsuji, Kenichi, Ichimoto, Kiyoshi, Asai, Ayumi
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 relationship between physical quantities (such as mass, kinetic energy
Externí odkaz:
http://arxiv.org/abs/2212.08850
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 Sun-as-a-star analyses of H$\alpha$ spectra for various active events
Externí odkaz:
http://arxiv.org/abs/2210.02819
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 magnetograph which scans the wavelength around a Fe I line at 6303 ang
Externí odkaz:
http://arxiv.org/abs/2208.10696
Stellar flares sometimes show red/blue asymmetries of H$\alpha$ line, which can indicate chromospheric dynamics and prominence activations. However, the origin of asymmetries is not completely understood. For a deeper understanding of stellar data, w
Externí odkaz:
http://arxiv.org/abs/2206.01395
Autor:
Namekata, Kosuke, Maehara, Hiroyuki, Honda, Satoshi, Notsu, Yuta, Okamoto, Soshi, Takahashi, Jun, Takayama, Masaki, Ohshima, Tomohito, Saito, Tomoki, Katoh, Noriyuki, Tozuka, Miyako, Murata, Katsuhiro L., Ogawa, Futa, Niwano, Masafumi, Adachi, Ryo, Oeda, Motoki, Shiraishi, Kazuki, Isogai, Keisuke, Seki, Daikichi, Ishii, Takako T., Ichimoto, Kiyoshi, Nogami, Daisaku, Shibata, Kazunari
Solar flares are often accompanied by filament/prominence eruptions ($\sim10^{4}$ K and $\sim 10^{10-11}$ cm$^{-3}$), sometimes leading to coronal mass ejections (CMEs) that directly affect the Earth's environment. `Superflares' are found on some act
Externí odkaz:
http://arxiv.org/abs/2112.04808
Autor:
Seki, Daikichi, Otsuji, Kenichi, Isobe, Hiroaki, Del Zanna, Giulio, Ishii, Takako T., Sakaue, Takahito, Ichimoto, Kiyoshi, Shibata, Kazunari
A filament, a dense cool plasma supported by the magnetic fields in the solar corona, often becomes unstable and erupts. It is empirically known that the filament often demonstrates some activations such as a turbulent motion prior to eruption. In ou
Externí odkaz:
http://arxiv.org/abs/2106.11875