Jon Eckberg's smoothy work directory : /disk/data/jeckberg/sxt_mov/

Descriptions for each video (years for reference, not part of description): 

1991.  Movie of the solar corona taken at soft x-ray wavelengths.  The
temperature of the hot coronal gasses depicted here are generally above 2
million degrees kelvin.  The movie begins in September 1991, closely following
the sunspot maximum of February 1989.  Solar activity was still high.

1992.  Movie of the solar corona, taken at soft x-ray wavelengths, covering
the steep activity decline of sunspot cycle 22.  Note the great decrease in
the brightness of the corona by the end of the video.  Even so, the brightest
coronal features are generally above 2 million degrees kelvin.  

1993.  Movie of the solar corona taken at soft x-ray wavelengths.  During this
year sunspot and coronal activity continues to decrease towards the minimum of
1996.

1994.  Movie of the solar corona taken at soft x-ray wavelengths.  Solar
activity is quite low but with sporadic outbursts.  The x-ray-bright active
regions now mostly appear quite near to the sun's equator.

1995.  Movie of the solar corona taken at soft x-ray wavelengths in the final
approach to sunspot minimum.  The general corona has cooled to temperatures
well below 2 million degrees kelvin so is faint in the SXT images.  Because of
the fainter corona and few bright active regions, the many so-called x-ray
bright points become visible everywhere on the disk.

1996.  Movie of the solar corona taken at soft x-ray wavelengths through the
minimum between activity cycle 22 and 23.  One side of the sun is nearly
devoid of activity, a single outburst of activity dominates the other side.
The x-ray corona is quite thin as compared to periods of higher activity.
This is a good time to observe the tiny x-ray bright points whose frequency is
fairly independent of sunspot numbers.

1997.  Movie of the solar corona taken at soft x-ray wavelengths during the
initial rise of activity cycle 23.  By the end of the year new-cycle active
regions, although still small, are appearing at solar latitudes of +/- 30
degrees.  The general corona is heating up to temperatures for which the 
SXT is more sensitive.

1998.  Movie of the solar corona taken at soft x-ray wavelengths as solar
activity increases -- evidenced by the larger number of x-ray-bright active
regions.  By the end of the year, the new active regions are appearing 
noticeably closer to the sun's equator.

1999.  Movie of the solar corona taken at soft x-ray wavelengths.  Several
"candle-flame" flare eruptions appear in the video.  Many x-ray loops
connecting active regions across the equator appear, especially towards 
the end of the year.

2000.  Movie of the solar corona taken at soft x-ray wavelengths in 2000 as
sunspot numbers and coronal activity reach a peak.  Large x-ray-dark coronal
holes reveal areas where the sun's magnetic fields are open to 
interplanetary space.  There is a dip in sunspot number around January 2001.

2001.  Movie of the solar corona taken at soft x-ray wavelengths in 2001.
X-ray emission is at 1998 levels for the first half of the year, increasing to
2000 levels by the end of SXT observations on 14 December 2001.

12. Movie of the solar x-ray corona from October 1991 (near the peak of
sunspot-cycle 22) to December 2001 (the peak of sunspot-cycle 23).  The solar
x-ray irradiance changes by nearly a factor of 1000 from maximum to minimum.
The temperature of the brightest parts of these images are generally above  2
million degrees Kelvin.

3.  Highly accelerated movie of the rotating solar x-ray corona from October
1991 to December 2001.  This video is intended to emphasize the coronal
effects of an entire solar activity cycle.  Note the annual "nodding" of the
solar poles of +/- 7 degrees.  The latitude drift toward the equator of active
regions is very evident.  The temperature of the hot coronal gasses depicted
here are generally above  2 million degrees Kelvin.