A collaborative team from the Harvard-Smithsonian Center for
Astrophysics, Goddard Space Flight Center and the Jet Propulsion
Lab, led by Shadi Habbal, will be carrying out photometric
observations of the corona in the visible wavelengths of the Fe
lines: 7892, 6374 and 5303 A. A CCD image of the corona taken in
6374 A during the eclipse of 24 October, 1995 in India is attached.
Data will be recorded on both CCD and photographic cameras. Polarization
measurements in the 5303 A line and in the white light will also be
made. The observations from Guadeloupe will be coordinated with
SOHO, VLA, and radio occultation measurements during the superior
conjunction of the spacecraft Galileo which is orbiting Jupiter.

The radio occultation measurements will probe the corona on a spatial
and temporal scale that cannot be achieved with imaging instruments. 
Members of the team include: S. R. Habbal, R. Esser, S. Fineschi and
A. Mossman (CfA), M. Guhathakurta and R. Fisher (Goddard/NASA),
J. Johnson (Electricon), M. Arndt (UNH) and R. Woo (JPL).

UVCS will support the NSF/SAO/GSFC expedition with measurements in the 
visible light (VL) and in the ultraviolet (UV). The UVCS VL channel
(VLC) will measure the polarized brightness pB of the K-corona between
1.8 Ro and 3.0 Ro. The two UV channell will be used to measure the
line profile of the Ly-alpha, -beta, OVI and SiXII doublets. 

The scientific objectives of the UVCS/Eclipse observations are:

- Electron density profile
- Calibration of the UVCS/VLC
- Electron temperature in streamers
- Elemental abundances 

The interpretation through the Hanle effect ("strong field regime") 
of the Green Line pB measurements taken during the expedition will be
used to derive the magnetic field geometry of the streamer boundaries.
The magnetic structure of streamers are suspected to determine the 
observed depletion of coronal heavy ions in their close loop region. 
(Raymond et al., ApJ; Noci et al, ESA) 

LASCO C2 and C3 will support the above expedition with pB measurements
in the white-light from 2.2-30 Ro, complementing the eclipse pB
observations from 1-2 Ro. LASCO C1 will provide Fe xiv (5303) and Fe x
(6374) line emissions for comparison with eclipse observations. Also
pB measurements of C1 (5303) will be used.

The scientific objectives of the LASCO/Eclipse observations are:

-Electron density profile
-Electron temperature in coronal holes, other isolated structures
-Magnetic field direction