1998 June-December
J.Singh, K.Ichimoto

1. A large number of raster scans were obtained in [Fe X] 6374 Angstrom,
[Fe XIV] 5303 Angstrom, [Fe XIII] 10747 Angstrom, and [Fe XI] 7892 Angstrom
coronal emission lines, choosing two lines simultaneously out of these four
with exposure times of 10-60 seconds, covering coronal regions of about
200 x 500 arcsec to study the variations in line parameters as a function
of height and to study the differences in the variations in line profiles
in open and closed; end-on and face-on; radial and  non-radial structures.

Paper:
Spectroscopic Studies of the Solar Corona II. Properties of Green
and Red Emission Lines in Open and Closed Coronal Structures
Singh,J., Sakurai,T. Ichimoto,K., Suematsu,Y., and Takeda,A.: 2002,
PASJ, 54, 793

2. Time sequence spectra were obtained at a fixed location in the solar
corona with the slit vertical to the limb with an exposure time of 6 
seconds to study the oscillations in the line parameters.

3. Time sequence spectra were obtained at two fixed locations separated by
50 arcsec in the solar corona with the slit vertical to the limb with
an exposure time of 10 seconds to study the oscillations in the line
parameters.

Paper:
Spectroscopic Observations of Coronal Waves
Sakurai,T. Ichimoto,K., Raju, K.P., and Singh,J.: 2002,
Solar Phys., 209, 265

4. Raster scans were obtained for 10747 and 10798 Angstrom emission lines
due to [Fe XIII] to study the density structure in the loops.

Paper:
Spectroscopic Studies of the Solar Corona III.
Density Diagnostics Using Infrared Lines of Fe XIII
Singh,J., Sakurai,T. Ichimoto,K., and Takeda,A.: 2002, PASJ, 54, 807