Engineering topics
Publications and source records attributed to Tousey, R..
Skylab XUV coronal spectroheliograms and photospheric magnetograms are compared. This comparison shows that, as new bipolar magnetic fields emerge through the solar surface into the corona, the new coronal fields interact with the old ones in a manner that suggests the reconnection of the field lines.
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The hydrogen Lyman-alpha emission line of comet Kohoutek (1973f) was observed and resolved by the high-dispersion Skylab/ATM S082B spectrograph shortly after the comet's perihelion passage (29-31 December 1973). The Lyman-alpha line width was determined from three different exposures of the comet nuclear region. A simplified analysis of the optical thickness effects showed that this line width is consistent with the established hydrogen outflow velocity of 8 to 10 km/sec.
Spectroheliograms obtained with the Naval Research Laboratory's Extreme Ultraviolet Spectrograph (S082A) on Skylab are compared with Kitt Peak National Observatory magnetograms. A principal result is the characteristic reconnection of flux from an emerging bipolar magnetic region to previously existing flux in its vicinity. Examples of the disappearance of magnetic flux from the solar atmosphere are also shown. The results of a particularly simple, potential field calculation are shown for comparison with the Skylab observations.
The extreme ultraviolet spectroheliograph of the Skylab-ATM experiment S082A recorded 1000 exposures during the mission, covering the wavelength range from 171 to 335 A or from 315 to 630 A. Each exposure recorded a spectrum of solar images with spatial resolution reaching 2 arc sec. Among the features observed were the chromospheric network, filaments, active regions, XUV bright points, the limb, spicules, prominences, coronal holes, and loops. During the mission, a number of flares were photographed; the images showed the changing form of a flare in different lines from the chromosphere to the corona as well as how this form changed during the course of the flare. The spectral images of a number of eruptive prominences were also recorded.
A TV image of the entire sun while an importance 2N solar flare was in progress was recorded in the extreme ultraviolet (XUV) radiation band 171-630 A and was transmitted to ground from an Aerobee-150 rocket on Nov. 4, 1969 using S-band telemetry. The camera tube was a SEC vidicon, with its fiber optic faceplate coated with an XUV-to-visible conversion layer of p-quaterphenyl. The XUV passband was produced by three 1000-A thick aluminum filters in series together with the platinized reflecting surface of the off-axis paraboloid that imaged the sun. A number of images were recorded with integration times between 1/30 sec and 2 sec. Reconstruction of pictures was enhanced by combining several to reduce the noise.
Solar UV flash spectrum by spectroheliographs flown aboard Aerobee 170 mission during total solar eclipse
Coronal observations from Aerobee 150 rocket after total solar eclipse of 7 March 1970 in Mexico, combining coronagraph flight record with ground photography
Extreme UV heliograms obtained by rocket-borne instruments to study excitation mechanisms of ionic resonance lines
Lunar crescent and earthshine at 2 degrees solar elongation, discussing occulted coronagraph photography, mean solar brightness and surface fluorescence
White light coronal streamers photographs obtained by rocket, noting geometry and coincidence with plages
Line identification methods in solar extreme UV and X ray regions
Analysis of coronal streamers photographed by white light coronagraphs flown on Aerobee 150 vehicle
Intensity studies on calcium-potassium plages and extreme ultraviolet spectroheliographs
High altitude Aerobee coronagraph and meteoritic dust tracks
Extreme UV emission, discussing chromospheric coarse mottling and network characteristics of He II 304 angstroms
Analyses of lunar crescent and earthshine observed at 2 deg solar elongation
Design of spectroheliograph to detect solar corona