Keiji HAYASHI

My interests/tasks

• MHD (magnetohydrodynamic) simulation study of global solar corona and solar wind, using the solar magnetic field data taken at SDO/HMI, SOHO/MDI, WSO, GONG, SOLIS and MWO. We use the IPS measurements, a remote-sensing technique measuring solar wind speed and density, at Nagoya University, Japan, to determine realistic solar wind speed boundary maps for the interplanetary simulations.
• Space-weather related topics : the global structure of the solar corona, solar wind and heliosphere, dynamic events such as coronal mass ejection, and the interplanetary disturbance propagation.
• Magnetic field and flow data, and data-pipeline processing of SDO/HMI.
  • An mpeg movie (20 MB) shows the three-component magnetic field at and nearby the sunspot region at AR 11057; this active region is the first one the HMI observed since its operation had started. Mind that the movie was made early May 2010, and the analysis and reduction were of preliminary version.
  • Another (mpeg, 115MB ; mp4 190MB) shows the evolution of the field at the east half of the AR 11158. An anaglyph provides a three-dimensional view at an instant.

• Our near-real time coronal MHD simulation using daily-updated SDO/HMI (an official page, *under construction!)
• MHD-derived/predicted solar corona; to-be-seen at the total eclipse on 2012 Nov. 13, 2010 July 11, 2009 July 22, and 2008 August 1. No TSE visible in 2011.
• Near real time solar wind maps by MHD tomography using IPS measurements (links to website at Solar Terrestrial Environment Lab. of Nagoya University, Japan), and a test page where I play (not regularly updated).

Recent/Forthcoming Publications/Presentations

• publication/presentation lists
• some of my abstracts to meetings/conferences/workshops

Others: movies, plots and brief descriptions of my works and related topics

• 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)
  • AniS 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
• sample FORTRAN 77 code for making PPM and BMP format files.

e-mail	:
phone	:
fax	:
postal address :
		Stanford University W. W. Hansen Experimental Physics Laboratory Solar Observatories Group 452 Lomita Mall, MC 4085, Cypress Hall C Stanford, CA 94305-4085
place of work :
		bldg. Cypress Hall C, 466 Via Ortega, Stanford, CA