Positron Annihilation Line from the 15 November 1991 Flare
Prominence Eruption in NOAA7125 on April 6, 1992
Reformation of a Coronal Helmet Streamer by Magnetic Reconnection after a Coronal Mass Ejection
Rotational Reversing Model and Triple Dipole Model as Substantiated by Yohkoh SXT Data
Small Scale Activity Just before the Onset of Radio Burst Detected by the Nobeyama Radioheliograph
Soft X-Ray Line Profiles Predicted by the Jet Model of Chromospheric Evaporation
Solar Abundances Derived from Gamma-Ray Line Spectroscopy of the 1991 October 27 Flare
Solar Flares as Ongoing Magnetic Reconection
Solar Image Processing and Feature Recognition
Solar Prominence Formation due to Current Loop Coalescence
Some Compact Flares Take Place in the Intersection of Magnetic Loops
Structure of The Soft X-Ray Corona and Its Effect to the Earth Quadrupole Type and Sea Anemone Type
Temperature and Density Structure of a Solar Flare Observed by the Yohkoh SXT and HXT
Temperature of Coronal Holes Measured by Yohkoh SXT
Temperature Structure of Active Regions Deduced from the Helium-Like Sulphur Lines
The Achievements of Yohkoh and The Next Solar Mission