|6/26||S.Ninomiya||upload or download|
|6/26||T.Sakaue||upload or download|
|13||7/3||Overall meeting of our observatories|
|Date||Name||Title||Abstract||File||4/10||K.Shibata||Solar Physics in Future 2017||pptx||4/17||S.Takeshige||I will introduce a paper, titled 'Spatial Growth of Current-driven Instability in Relativistic Rotating Jets and the Search for Magnetic Reconnection', Singh et al. 2016. http://adsabs.harvard.edu/abs/2016ApJ...824...48S||4/17||A.Asai||A 3-dimensional view of a filament eruption and CMEs associated with the 2011 March 8 Solar Flare||pptx||4/24||K.Ichimoto||I will give an overview of the Solar observation projects in 2017.as usual at the beginning of the fiscal year.|
- Solar-C status
- What we do at Hida?
|5/1||Y.Notsu||"A solar-like magnetic cycle on the mature K-dwarf 61 Cygni A (HD 201091)"||
In the short talk on next Monday, I will introduce the following paper.
"A solar-like magnetic cycle on the mature K-dwarf 61 Cygni A (HD 201091)"
Boro Saikia et al. 2016, A&A, 594, 29
This paper reports the first detection of a cool star, apart from the Sun, where the magnetic cycle (polarity reversal etc) is in phase with its chromospheric cycle (Ca II intensity changes), on the basis of 8-year spectropolarimetric monitoring observations.
|5/1||S.Ueno||In the tomorrow's solar seminar, I plan to talk about the following two things. 1) Introduction of the theme of Mr. Kaiho's DST-observation in last week: According to Ishii-san, Director Shibata requested that contents of recent DST observations should be introduced in the solar seminar. So, I received Mr. Kaiho's presentation file for the seminar on Apr-25. I will briefly introduce it again for people who could not attend his seminar. 2) Report of conference about Chinese future ground-based solar telescopes: When we visited Fuxian Solar Observatory in last December, I attended the conference about Chinese future solar telescopes in Kunming. In this conference, the Chinese Giant Solar Telescope (CGST) and 2.5 m solar and stellar telescope (ISMART) were mainly treated. I will report outline of this conference.||5/8||K.Hirose||5/8||A.Kawamura||Statistical Characteristics of Solar cycle 23 & Newly Found Aurora Picture (of Solar Cycle 19)||5/15||U.Kou||Statistical Characteristics of Solar cycle 23 & Newly Found Aurora Picture (of Solar Cycle 19)||Today I will have a brief introduce of Title: Magnetic Field and Plasma Diagnostics from Coordiated Prominence Observations Author: B. Schmieder et. al Link: http://adsabs.harvard.edu/abs/2016ASPC..504..119S Abstract: This paper studies the temperature, density and flow velocities of the prominence from a statistical point of view by combining the measurements from THEMIS, IRIS, HINODE/EIS and Meudon Solar Tower. They are aiming to answer the following question: 1. what is the general direction of the magnetic field in prominences? 2. are prominences in a weak environment field dominated by gas pressure? 3. if there are substantial velocities to maintain vertical rotation structures, as has been suggested for tornado-like prominences.!--||5/15||S.Nagata||5/22||5/29||K.Namekata||5/29||S.Ninomiya||6/5||D.Cabezas||In tomorrow's seminar as a short talk, I will introduce the paper by Kleint et al. (2015) entitled as: "The fast filament eruption leading to the X-flare on 2014 March 29" http://adsabs.harvard.edu/abs/2015ApJ...806....9K||6/5||T.Anan||Which spectral line is good for future Japanese space missions?||I would like to talk about development of simultaneous multi-spectral windows spectropolarimetry of the Domeless Solar Telescope at Hida Observatory to select which spectral line is good for future Japanese space missions. At the end of presentation, I would like to discuss with you science objectives what you want to study using the polarimetry.||6/12||K.Otsuji||Which spectral line is good for future Japanese space missions?||In next monday's seminar as a short talk, I will introduce the papers shown below: "On HMI solar oblateness during solar cycle 24 and impact of the space environment on results" Meftah, M.; Hauchecorne, A.; Bush, R. I.; Irbah, A. Advances in Space Research, Volume 58, Issue 7, p. 1425-1440. http://ads.nao.ac.jp/abs/2016AdSpR..58.1425M||pptx||6/12||H.Isobe||gFlux rope seismology for diagnosing the eruption onset.h||The references are: Forbes 1990, JGR, 95, 11919 Isobe & Tripathi 2006, A&A, 449, L17 Isobe, Tripathi, Asai & Jain 2007, Sol. Phys. 246, 89 Pinter, Jain, Tripathi & Isobe 2008, ApJ, 680, 1560 Foullon, Verwichte, & Nakariakov 2009, ApJ, 700, 1658 Joshi et al. 2016, ApJ, 833, 243 I will also show some results of MHD simulation of flux rope oscillation with changing the parameters that control the flux ropefs (loss of) equilibrium.||pptx||6/19||H.Tamazawa||In today's seminar as as short talk, I will introduce the paper shown below, "Atmospheric impace of the strongest known solar particle storm of AD 775" Sukhodolov et al. 2017 Scientific Reports, 7, 45257||pptx||6/19||Elena Kupriyanova|
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