These are individual composite images from the previous graphic.  The
EUV emission from the extended corona comes from O VI.   Artificial
eclipses produced by UVCS block out the disk of the Sun and filter
out everything except the O VI 1032 Angstrom emission.
Sometimes UVCS scans the extended corona in a ``synoptic''
sequence.  For this standard observation, the UVCS instrument
observes a narrow rectangle in the solar corona that is 40
arcminutes long and 84 arcseconds wide.  The rectangle can be
scanned in height at each of eight position angles around the Sun.
The images are made by interpolating between positions to provide
complete coverage between the inner and outer heights.  The
composites have been generated from five UVCS/SOHO and EIT/SOHO
synoptic images taken in May 1996, May 1997, May 1998, May 1999,
and May 2000, covering over four years of SOHO's operation.  The
histogram shows the number of sunspots from mid-1995 through
September 2000.  The corona displays a variety of features
including coronal holes and streamers.  In the above images,
those features and the overall shape and brightness of the corona
can be seen changing with the sunspot activity cycle.  From solar
minimum in 1996 to mid-1998, the large scale configuration of the
corona consists of dark coronal holes over the north and south
heliographic poles and quiescent streamers at the equator.  Toward
solar maximum, there is a striking difference in the appearance of
the corona.  The streamers fill more of the coronal volume, and the
extended corona and disk become considerably brighter.