Most of this occurred at NASA/Marshall Space Flight Center in the (now defunct) Space Sciences Laboratory in Huntsville, Alabama, 100mi north of Birmingham.
What you see to the left is a Transmission Electron Micrograph (TEM) of a cross section of several thin layers put down via RF triode sputtering. The bottom dark area is the silicon wafer substrate. The alternating white and grey areas are silver and silicon, respecitively. A standard silver-silicon pair is approximately 15nm thick.
Above that is the epoxy used to create the TEM sample.
The structure is comprised of two multilayer mirrors, each consisting of seven pairs of silver-silicon layers. They are face to face across a thicker silicon ``spacer'' and the system can be described as a Fabry-Perot Etalon.
Dr. Palmer N. Peters worked with me to create these narrow band-pass filters for use in the soft xray. These filters could, in theory, be used for visible light rejection and spectral line selection for the MSSTA telescopes (described below).
This telescope array consits of at least fourteen different telescopes each coated with various multi-layer coatings optimized for imaging various extreme ultraviolet (EUV) wavelengths.
The 1994 flight, on 1994 November 03, 19:15 UT, carried a total of nineteen telescopes (which I got the dubious honor of focussing and aligning!). Six were Ritchey-Chrétien telescopes, and two were of Cassegrain design. The remaining eleven telescopes were Herschellians.
The first flight, on 1991 May 13, 19:03 UT, carried seven Ritchey-Chrétien, two Cassegrain, and five Herschellian telescopes. I was present for most of the photographic work which followed this flight.
In conjunction with observing and recording EUV emissions from the sun, I worked with Allen Gary on theoretically calculating and modeling expected EUV radiation by:
|retrieving magnetograms from the Kitt Peak Solar Vacuum Telescope,|
|calculating B field lines and flux tubes in the active regions, and guessing at plasma densities and energies.|
|The goal of this work is to compare the theoretical EUV emissions from within these flux tubes with the data gathered from the MSSTA flights (described above) and images like this from YOHKOH.|