Solar Seminar (Zasshikai) Home Page (FY2017)


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

News
The next seminar will start from 13:00 on Dec. 18th (Mon).
  • Useful webpage list for solar observers.
  • See also Ishii-san's Webpage and Webpage of Kwasan and Hida Observatories.
  • Next presenters

    Date Time Section Speaker File
    2017-12-18 13:00-14:00
    D2 interim
    Y.Notsu 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

    Presentations in this semester

    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
    12-25
    short
    S.Okada
    12-25
    main
    S.Tokuda



    Previous presentations

    2017-1st Zasshikai Website
    Go to Zasshikai 2017-1st
    2016 Zasshikai Website
    Go to Zasshikai 2016
    2015 Zasshikai Website
    Go to Zasshikai 2015
    All of 2014
    2014 Archive (tar.gz file, 1.9Gbyte)
    All of 2013
    2013 Archive (tar.gz file, 2.4Gbyte)
    All of 2012
    2012 Archive (tar.gz file, 780Mbyte)
    All of 2011
    2011 Archive (tar.gz file, 780Mbyte)
    All of 2010
    2010 Archive (tar.gz file, 625Mbyte)



    If there are any mistakes or errors in this webpage,
    please send e-malis to the organizer, Huang Y.W (kouui_at_kwasan.kyoto-u.ac.jp).