|2017-12-18||13:00-14:00||Y.Notsu||upload or download|
|Date||Name||Title||Abstract||File||10-02||S.Ueno||introduction of some examples of recent Indian group's studies using long-term Kodaikanal full-disk CaII K digitized data||
"A BUTTERFLY DIAGRAM AND CARRINGTON MAPS FOR CENTURY-LONG Ca II K SPECTROHELIOGRAMS FROM THE KODAIKANAL OBSERVATORY"
Subhamoy Chatterjee, Dipankar Banerjee, and B. Ravindra
2016, ApJ 827, 87
"Association of Plages with Sunspots: A Multi-Wavelength Study Using Kodaikanal CaII K and Greenwich Sunspot Area Data"
Sudip Mandal, Subhamoy Chatterjee, and Dipankar Banerjee
2017, ApJ 835, 158
"Long-term Variations in the Intensity of Plages and Networks as Observed in Kodaikanal Ca-K Digitized Data"
Muthu Priyal, Jagdev Singh, Ravindra Belur, Somasundaram Kameshwaran Rathina
2017, Sol.Phys. 292, 85
"Variation of Supergranule Parameters with Solar Cycles: Results from Century-long Kodaikanal Digitized CaII K Data"
Subhamoy Chatterjee, Sudip Mandal, and Dipankar Banerjee
2017, ApJ 841, 70
"ASSOCIATION OF SUPERGRANULE MEAN SCALES WITH SOLAR CYCLE STRENGTHS AND TOTAL SOLAR IRRADIANCE"
SUDIP MANDAL, SUBHAMOY CHATTERJEE, DIPANKAR BANERJEE
2017, ApJ, accepted on May 31
|10-02||P.Heinzel||10-16||A.Asai||introduction of a just published paper||
"Variation of the Solar Microwave Spectrum in the Last Half Century"
by M. Shimojo, K. Iwai, A. Asai, S. Nozawa, T. Minamidani, and M. Saito
2017, Astrophysical Journal, Vol. 828, Number 1, id 62
||10-23||T.Sakaue||introduction of Czesla et al. 2012 A&A||
Title: The extended chromosphere of CoRoT-2A. Discovery and analysis of the chromospheric Rossiter-McLaughlin effect
Authors: Czesla, S.; Schröter, S.; Wolter, U.; von Essen, C.; Huber, K. F.; Schmitt, J. H. M. M.; Reichart, D. E.; Moore, J. P.
flare study :
"Opacities of the Mg II h & H-alpha lines and Interpretation of the Mg II h line shape"
|10-30||S.Nagata||10-30||K.Otsuji||Observational summary of September 2017 major flares at NOAA12673||
NOAA 12673 was a simple unipolar region when it rotated from the limb, but an emerging flux region appeared on Sep. 2 then it rapidly developed into a beta-gamma-delta type sunspot configuration. It produced many >M class flares including X9.3 on Sep. 6, which is the biggest flare for this solar cycle. The PSTEP member analyzed a various data of that flares, and I will introduce the initial result and summary of the analysis.
Spectro-polarimteric studies of Sunspot and its fine-structure
Spectro-polarimetry is the key to understand the physical properties of the solar atmosphere. At Udaipur Solar Observatory (USO), an imaging spectro-polarimeter has been developed to carry out the simultaneous spectro-polarimetric (SP) observations of the photosphere (Fe I 617.3 nm spectral line) and chromosphere (Ca II 854.2 nm). In this talk, I will present the details of a new Milne-Eddington inversion code (named as SPIN) developed specifically to invert SP data of Multi-Application Solar Telescope (MAST). I will also discuss the details of tests performed to validate the SPIN code and its application to inverting the MAST/SP data. In addition to this, physical properties of umbral dots using high-resolution G-band images obtained from Hinode space-based telescope will be discussed. I will also discuss the relationship between the umbral dots and macro-properties of the sunspots.
|11-27||H.Isobe||About e-p annihilation line in the flaring solar atmosphere||
the detection of electron-positron annihilation line from lightenings
the mechanism of e-p annihilation line in the flaring solar atmosphere
Title : "The Physics of Positron Annihilation in the Solar Atmosphere"
R. J. Murphy, G. H. Share, J. G. Skibo, and B. Kozlovsky, ApJS, 161:495-519 (2005)
|pptx||11-27||D.Seki||ambient potential magnetic field of the filament@2016/11/05||
title : The magnetic field surrounding the filament erupted on 2016 Nov. 5th
abstract : One of the keys to explain the cause or the trigger of a filament eruption is torus instability. Since the outward-directed hoop force in current ring (filament) decreases when the ring expands, a perturbation will be unstable if the opposing Lorentz force due to potential fields surrounding the filament decreases faster with increasing R than the hoop force (Kliem+2006). From this point of view, I investigated the potential field around the filament which erupted on 2016 Nov. 5th calculated by CIDAS system from 2016 Nov. 2nd to 5th. As a result, the potential field over the filament apparently decreased, and the eruption may be triggered by the torus instability.
|12-04||T.Anan||a report of DKIST critical science plan workshop||
DKIST critical science plan workshop
I attended the DKIST critical science plan workshop in Huntsville to develop plan, which defines critical science goals for the first two years of DKIST operations. The plan will be converted into observing proposals. In this seminar, I introduce the DKIST, some science goals proposed in the workshop. I recommend you to attend next workshop in Feb. 26-28, 2018 at Nagoya to propose your science plan with the DKIST.
|12-04||K.Namekata||research about star spot||12-11||A.Kawamura||paper introduction||
G. Steward, V. Lobzin, I. H. Cairns, B. Li, & D. Neudegg (2017)
Automatic recognition of complex magnetic regions on the Sun in SDO magnetogram images and prediction of flares: Techniques and results for the revised flare prediction program Flarecast
Space Weather, Volume 15, Issue 9, pp1151-1164
Dynamics Processes of the Moreton Wave on 2014 Mach 29
In my talk I will present progress and preliminary results of my current research work, that relates to the Moreton wave observed by the Flare Monitoring Telescope (FMT) in operation at Ica National University, Peru.
Using Ha wing observations (-/+0.8 Angstrom) we estimated the Doppler velocity of the Moreton wave, expressed in terms of perturbation profile. I will present this result and discuss the fact in which the Moreton wave is created under the action of the wave propagation in the Corona.
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