These are fully calibrated polarization brightness images created by scanning the corona
at 1/2 degree intervals and sampling the entire corona every 3 minutes. The data are in the original (native) coordinate
system and are ideal for azimuthal and radial scans. Polarization brightness data are required for measuring coronal densities
and computing masses.
These images are the fully calibrated polarization brightness images shown above but with a coordinate transformation
applied to depict the data in the standard rectangular coordinate system. Some interpolation is required and increases
with increasing solar radius. Polarization brightness data are required for measuring coronal densities and computing masses.
Qualitative white light coronal images. These images have had an artificial vignetting function applied which reduces
the radial density gradient in order to enhance contrast. These data are ideal for measuring positions of coronal mass
ejections (CMEs), streamer locations and other coronal structures. They are not for measuring densities or mass.
The jpegs are made from these images.
ACOS CHIP Helium I 1083 nm intensity data provide a good indication of large scale structures in the upper chromosphere
and corona including active regions, prominences and filaments, filament channels, and coronal holes. Intensity images
are obtained by subtracting a nearby continuum image from an image taken at HeI line center.
ACOS CHIP Helium 1083 nm velocity data are obtained by subtracting images taken in the blue and red wings of the HeI line
and provide qualitative velocity information.
PICS H-alpha disk data provide information about prominence and filament activity and eruptions, moreton waves, and optical flares.
These images have a limb-darkening correction applied as well as some contrast enhancement.
PICS H-alpha disk data provide information about prominence and filament activity and eruptions, moreton waves,
and optical flares. These images have had minimal processing: no flat-fielding or limb darkening corrections are applied.
PICS H-alpha limb data are taken with a broad 0.9 nm filter and provide views of the solar limb
activity by occulting the solar disk. These data are ideal for tracking the motions of erupting and active prominences to
large heights. No corrections are applied to these data.
