Keiji Hayashi

• MHD (magnetohydrodynamic) simulation study of solar corona and solar wind
• solar photospheric magnetic field data and other solar/interplanetary data as the input for the simulation
• space weather related issues such as the global coronal structures, the coronal mass ejection, and the interplanetary disturbance propagation

• Daily coronal MHD simulation : Click here to find figures and plots of my quasi-real time coronal MHD simulation using daily-updated SOHO/MDI data. 1 AM begins the routine job that gets MDI data via http, processes the data, and starts the time-relaxation MHD simulation. New plots are generated around 7 AM (pacific time).
• Prediction of solar corona at the total eclipse, August 01, 2008. (clike here)
• MHD tomography for IPS observation of the solar wind : The tomographic reconstructions of the solar wind from the IPS (Interplanetary radio Scintillation) measurement, including MHD version, are available at webpage at STEL/Nagoya University.

Recent/Forthcoming Publications/Presentations

• "An MHD simulation model of the global solar corona with the time-varying boundary magnetic field based on the measurement data", Keiji Hayashi, SPD/AGU joint assembly 2008 (#SH51B-02), 27--30 May 2008 / Fort Lauderdale, FL
• "Validation of Two MHD Models of the Solar Corona with Rotational Tomography", Alberto M. Vasquez, Richard A. Frazin, Keiji Hayashi, Igor V. Sokolov, Ofer Cohen, Ward B. Manchester IV, and Farzad Kamalabadi, ApJ (2008) Vol.682, 1328-1337
• "MHD Simulations of the Global Solar Corona around the Halloween Event in 2003 Using the Synchronic Frame Format of the Solar Photospheric Magnetic Field", Keiji Hayashi, Xue Pu Zhao, and Yang Liu, JGR (2008) Vol.113, A07104, doi:10.1029/2007JA012814
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  publication/presentation lists (2003∼)
  some of my abstracts to meetings/conferences/workshops

Gallery : movies, plots and brief descriptions of my works and interests

• gallery contents
  • MHD simulation of solar wind / corona
    brief descriptions on other models of solar wind / corona (the Parker solution, and so on)
  • test simulation (Orszag-Tang vortex, shock tube etc.)
  • visualization (contour-surface drawing, volume rendering, and line-of-sight integration of 3D data)
  • java-applet animation
    • Friedrichs diagram (phase velocity of MHD waves)
    • MHD wave propagation in aligned magnetic fields (group velocity)
    • spherical harmonics for calculation of solar surface magnetic field (∼1.6MB).
• sample FORTRAN 77 code for making PPM and BMP format file.

e-mail	:
phone	:
fax	:
postal address :
		Solar Physics Group W. W. Hansen Experimental Physics Laboratory Stanford University Cypress C 491 South Service Road Stanford, CA 94305-4085