Skylab Ultraviolet Stellar Astronomy ~ 1973 NASA; UV Photo Spectroscopy of Stars; Karl Henize

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“The objectives of this experiment were to take UV photographs of young and hot stars, nebulae, interstellar dust, and stellar gas shells in large areas of the Milky Way, and evaluate large numbers of spectra for spectral classes, temperatures, and compositions of stars, using a reflecting telescope and an objective prism in front of a 35 mm camera. The telescope had a 15-cm reflecting mirror. Several different prisms could be inserted in front of the telescope, depending on the desired spectral resolution and sensitivity. The instrument was sensitive in the spectral region from 1400 to 3000 A. The instrument was mounted in the antisolar airlock of the orbital workshop, and the telescope looked at different portions of the sky by means of a movable flat mirror. Photographs were taken only while Skylab was on the dark side of its orbit. The image of each star was drawn out into a small spectrum. About fifty 4 x 5 deg star fields were observed during each of the three Skylab missions. Details could be resolved to about 20 arc-s. Films were developed and evaluated on the ground. For more details, see F. G. O’Callaghan, K. G. Henize, and J. D. Wray, App. Opt., v. 16, p. 973, 1977”

Public domain film from NASA, slightly cropped to remove uneven edges, with the aspect ratio corrected, and one-pass brightness-contrast-color correction & mild video noise reduction applied.
The soundtrack was also processed with volume normalization, noise reduction, clipping reduction, and/or equalization (the resulting sound, though not perfect, is far less noisy than the original).

Ultraviolet astronomy is the observation of electromagnetic radiation at ultraviolet wavelengths between approximately 10 and 320 nanometres; shorter wavelengths—higher energy photons—are studied by X-ray astronomy and gamma ray astronomy. Light at these wavelengths is absorbed by the Earth’s atmosphere, so observations at these wavelengths must be performed from the upper atmosphere or from space.

Ultraviolet line spectrum measurements are used to discern the chemical composition, densities, and temperatures of the interstellar medium, and the temperature and composition of hot young stars. UV observations can also provide essential information about the evolution of galaxies.

The ultraviolet Universe looks quite different from the familiar stars and galaxies seen in visible light. Most stars are actually relatively cool objects emitting much of their electromagnetic radiation in the visible or near-infrared part of the spectrum. Ultraviolet radiation is the signature of hotter objects, typically in the early and late stages of their evolution. If we could see the sky in ultraviolet light, most stars would fade in prominence. We would see some very young massive stars and some very old stars and galaxies, growing hotter and producing higher-energy radiation near their birth or death. Clouds of gas and dust would block our vision in many directions along the Milky Way.

The Hubble Space Telescope and FUSE have been the most recent major space telescopes to view the near and far UV…

Charles Stuart Bowyer is generally given credit for starting this field…

Karl Gordon Henize, Ph.D. (17 October 1926 – 5 October 1993) was an American astronomer, space scientist, NASA astronaut, and professor at Northwestern University. He was stationed at several observatories around the world, including McCormick Observatory, Lamont-Hussey Observatory (South Africa), Mount Wilson Observatory, Smithsonian Astrophysical Observatory and Mount Stromlo Observatory (Australia). He was in the Astronaut Support Crew for Apollo 15 and Skylab 2, 3 and 4. As a Mission Specialist on the Spacelab-2 mission (STS-51-F), he flew on Space Shuttle Challenger in July/August 1985. He was awarded the NASA Exceptional Scientific Achievement Medal in 1974.

He died in 1993, during a Mount Everest expedition. The purpose of this expedition was to test for NASA a meter called a Tissue Equivalent Proportional Counter (TEPC): testing at different altitudes (17,000 ft, 19,000 ft and 21,000 ft) would reveal how people’s bodies would be affected, including the way bodily tissues behaved, when struck by radiation, and this was important for the planning of long duration space missions. Having reached Advanced Base Camp at 21,300 feet (6,500 m), the expedition was cut short when Henize died from high altitude pulmonary edema (HAPE) on October 5, 1993…


RonJohn63 says:

9:16 Proof that NASA is hiding Reptilians from Nibiru!!

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