Zobrazeno 1 - 10
of 144
pro vyhledávání: '"Ishii, Takako T"'
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:
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
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
It is widely recognised that filament disappearances or eruptions are frequently associated with Coronal Mass Ejections (CMEs). Since CMEs are a major source of disturbances of the space environment surrounding the Earth, it is important to investiga
Externí odkaz:
http://arxiv.org/abs/2102.04578
Autor:
Gutierrez, Maria V., Otsuji, Kenichi, Asai, Ayumi, Terrazas, Raul, Ishitsuka, Mutsumi, Ishitsuka, Jose, Nakamura, Naoki, Yoshinaga, Yusuke, Morita, Satoshi, Ishii, Takako T., UeNo, Satoru, Kitai, Reizaburo, Shibata, Kazunari
We present a detailed three-dimensional (3D) view of a prominence eruption, coronal loop expansion, and coronal mass ejections (CMEs) associated with an M4.4 flare that occurred on 2011 March 8 in the active region NOAA 11165. Full-disk H$\alpha$ ima
Externí odkaz:
http://arxiv.org/abs/2101.08575
Autor:
Seki, Daikichi, Otsuji, Kenichi, Ishii, Takako T., Hirose, Kumi, Iju, Tomoya, UeNo, Satoru, Cabezas, Denis P., Asai, Ayumi, Isobe, Hiroaki, Ichimoto, Kiyoshi, Shibata, Kazunari
This paper describes a new SMART/SDDI Filament Disappearance Catalogue, in which we listed almost all the filament disappearance events that the Solar Dynamics Doppler Imager (SDDI) has observed since its installation on the Solar Magnetic Activity R
Externí odkaz:
http://arxiv.org/abs/2003.03454
Autor:
Seki, Daikichi, Otsuji, Kenichi, Isobe, Hiroaki, Ishii, Takako T., Ichimoto, Kiyoshi, Shibata, Kazunari
Filaments, the dense cooler plasma floating in the solar corona supported by magnetic fields, generally exhibit certain activations before they erupt. In our previous study (Seki et al. 2017 ), we observed that the standard deviation of the line-of-s
Externí odkaz:
http://arxiv.org/abs/1902.08718