Solar Seminar home page (FY2017)

Solar Seminar (13:00-15:00 Monday, Room 504 5th floor building 4) Access

Upcoming

practice for 2018 Spring Annual Meeting, date to be decided

Clette-san's sepcial seminar on 03/27 14:00-16:00

Useful webpage list for solar observers.

Next presenters

Date	Time	Section	Speaker	File
				upload or download
				upload or download

For Speakers

Presentation time for speaker is: main : 40 minutes as a guide, and 20 minutes discussion.
short : 20 minutes as a guide, and 10 minutes discussion.
Contents of talk are: main : about your study
short : review of recent interesting paper and share information of recent study of the Sun.
Language of slide and talks: Master cource students : Language of slide and talk could be Japanese
Doctor cource students and over : Slide must be English, and talking language could be Japanese
(If those who could not understand Japanese attend the seminar, it is preferable that you talk in English)
Title and Abstract: Please send the title and abstract of your presentation by the day before.
Presentation files: Please upload your presentation files by the start of the seminar.
If the presentation file is very big, please zip the file before uploading.

For Audiences

Honoring speakers: Plase clap your hands as a closure of a presentation to express your respection to a speaker.

For everyone

Publication sharing: Please send a copy of the submitted version of any paper on which they are working to the zasshikai mailing list just after submission

Main speaker
Shibata, Ichimoto, Nagata, Ueno, Asai, Ishii, Nishida, Otsuji, Anan, Isobe,
Tamazawa, Kawamura, Takeshige, Notsu, Hirose, Denis, Kou, Sakaue, Tei,
Nakamura, Namekata, Ninomiya, Seki, Machida, Okada, Tokuda
Short speaker
Shibata, Ichimoto, Nagata, Ueno, Asai, Ishii, Nishida, Otsuji, Anan, Isobe,
Tamazawa, Kawamura, Takeshige, Notsu, Hirose, Denis, Kou, Sakaue, Tei,
Nakamura, Namekata, Ninomiya, Seki, Machida, Okada, Tokuda

Date		Name	Title	Abstract	File
10-02	short	S.Ueno	introduction of some examples of recent Indian group's studies using long-term Kodaikanal full-disk CaII K digitized data	References: "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	Guest	P.Heinzel
10-16	short	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 DOI: https://doi.org/10.3847/1538-4357/aa8c75	pptx
10-16	main	A.Machida	Determination of the wave property in the quiescent prominence Study about the velocity field of the Arch Filament System	From the spectroscopic observation with Domeless Solar Telescope at Hida Observatory, we found a wave in Doppler velocity and temperature of a prominence. I will discuss the possible property of the wave. We are now applying Becker's cloud model (the code was developed by Otsuji-san) to Arch Filament Systems in order to calculate the velocity field. I will introduce this study and discuss the relation between the velocity field and the geometry of the AFS.	pdf
10-23	short	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. ADS: http://adsabs.harvard.edu/abs/2012A&A...539A.150C
10-23	main	A.Tei	flare study : "Opacities of the Mg II h & H-alpha lines and Interpretation of the Mg II h line shape"		pdf
10-30	short	S.Nagata
10-30	main	K.Otsuji	Observational summary of September 2017 major flares at NOAA12673	Abstract: 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.	pptx
11-13	Guest	Y.Rahul	Research report	Title: Spectro-polarimteric studies of Sunspot and its fine-structure Abstract: 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	short	H.Isobe	About e-p annihilation line in the flaring solar atmosphere	the detection of electron-positron annihilation line from lightenings https://arxiv.org/pdf/1711.08044.pdf 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) http://iopscience.iop.org/article/10.1086/452634	pptx
11-27	main	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.	pdf
12-04	short	T.Anan	a report of DKIST critical science plan workshop	Title: DKIST critical science plan workshop Abstract: 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.	pdf
12-04	main	K.Namekata	research about star spot		pdf
12-11	short	A.Kawamura	paper introduction	Author: G. Steward, V. Lobzin, I. H. Cairns, B. Li, & D. Neudegg (2017) Content: 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 DOI: 10.1002/2017SW001595	pdf
12-11	main	D.Cebezas	research report	Title: 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.	pdf
12-18	D2 interim presentation	Y.Notsu			pdf
12-25	short	S.Okada	paper introduction	Title: "The magnetic field configuration of a solar prominence inferred from spectropolarimetric observations in the He i 10 830 Å triplet" D. Orozco Suarez+2014 https://www.aanda.org/articles/aa/pdf/2014/06/aa22903-13.pdf
12-25	main	S.Tokuda	paper introduction	Title: "Characteristics of Transverse Waves in Chromospheric Mottles" Authors: D.Kuridze, G.Verth, M.Mathioudakis, R.Erdelyi, D.B.Jess, R.J.Morton, D.J.Christian, and F.P.Keenan (The Astrophysical Journal, Volume 779, Issue 1, article id. 82, 8 pp. (2013)) DOI:10.1088/0004-637X/779/1/82	pdf
01-15	Master presentation (beta)	T.Nakamura
01-15	Master presentation (beta)	S.Ninomiya
01-29	Master presentation (beta)	K.Namekata
02-05	short	T.Ishii	Solar activity in 2017		pptx
02-05	main	Y.Huang		Basics of Digital Camera sensor (CCD/CMOS) and experiments of the infrared CMOS sensor in NAOJ for the purpose of polarization observation.
TBD	practice for 2018 Spring Annual Meeting	TBD
03-27	special seminar	Clette-san