Sixteen 25-pixel windows will be observed with the NIS, using the 4x240arcsec slit and 30s exposures. Fe XI 353, and Fe XIV 354. During the flight, emphasis will be on the target regions and in particular on Target 2. Measurements will be made of the integrated 304A solar flux during the flight with the Solar Extreme Ultraviolet Monitor. We invite ALL observers to participate with collaborative observations.
Primary targets are the north polar hole and the streamer belt surrounding the polar coronal holes.
The White Light Coronagraph determines the distributions of electron density from polarized radiance and absolute radiance observations of closed and open magnetic structures between 1.25 and 6 solar radii from sun center. The WLC is the most recent version of the space-borne externally occulted Lyot coronagraph, whose predecessors include experiments flown by HAO on balloons, the Skylab Apollo Telescope Mount, sounding rockets, and the Solar Maximum Mission. WLC uses a rotating half-wave plate, a linear polarizer, a serrated occulting disk for occulting the disk at 1.25 solar radius, and a linear, wide dynamic range detector CCD camera to measure the intensity and polarization of broad band visible coronal radiation. Observations out to 6 solar radii from sun-center will be obtained within a sector of 60 degrees in width centered on the UVC radial scan capability. Coordinates for the targets will be announced 28 hours before deployment.