Observations on man in an oxygen-helium environment at 380 mm. Hg total pressure. III - Heat exchange.
Thermal balance and heat exchange between four men exposed to helium-oxygen atmosphere at 380 mm Hg total pressure
ENVIRONMENTAL TESTING↗
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Search indexed NASA NTRS and DOE OSTI research on propulsion, heat transfer, battery materials and energy systems. Follow report and document links to the original sources.
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Observations of the lunar eclipse of December 19, 1964, at a wavelength of 3.3 mm.
Radiometric observations of total lunar eclipse of December 19, 1964 at wavelength of 3.3 mm indicate no significant temperature difference
RADIOMETRY↗
Detailed study of contaminant production in a space cabin simulator at 760 mm of mercury.
NASA and USAF experiment on mans contribution to trace contaminants in space cabin simulator at 760 mm of Hg
SPACE CABIN SIMULATOR↗
The galactic radio source W49 at 3.4 mm.
Galactic radio source W49 at 3.4 mm, showing no additional components in spectrum with turnover points at various frequency ranges
GALACTIC RADIO WAVE↗
Contaminant concentrations in a space cabin simulator at 258 mm Hg.
Contaminant concentration due to human habitation of space cabin simulator at 258 mm Hg and oxygen atmosphere environment
SPACE CABIN SIMULATOR↗
Mm-wave power meter mount
E-band thermistor mount and a technique for adjusting a temperature compensating thermistor to provide an electrically balanced bridge are used for measuring RF power in the mm-wavelength. The mount is relatively insensitive to temperature effects that cause measurement errors in single ended circuits.
Mullen, D. L.↗
Observations on man in an oxygen-helium environment at 380 mm. Hg total pressure. IV.
Human speech intelligibility and physical characteristics in O-He environment at 380 mm Hg, noting increase in formant frequencies
Endicott, J. E.↗
On the interpretation of Mercury observations at wavelengths of 3.4 and 19 mm.
Microwave observations of Mercury at 3.4 and 19 mm, interpreting brightness temperature variation with phase angle with basically lunar model
Morrison, D.↗
Radiometric measurement of attenuation and emission by the earth's atmosphere at wavelengths from 4 cm to 8 mm.
Radiometric measurement of attenuation, emission and noise fluctuations due to earth atmosphere in 4 cm to 8 mm range
Brown, W. E., III↗
Upper limits to the intensity of background radiation at lambda equals 1.32, 0.559, and 0.359 mm.
Background radiation intensity upper limits for mm and submillimeter wavelengths in interstellar medium, noting intense flux in far IR
Bortolot, V. J., Jr.↗
In-flight calibration of the Apollo 14 500 mm Hasselblad camera
In-flight calibration of 500-mm Hasselblad camera flown on Apollo 14
Kenefick, J. F.↗
The linear polarization of lunar thermal emission at 3.1 mm wavelength
Several observations of the distribution of linearly polarized lunar thermal emission were made at a wavelength of 3.1 mm with 4.88 m parabolic reflector from February to March 1971. A shadow corrected rough surface thermal emission model was least squares fitted to the data. Results indicate an effective lunar dielectric constant of 1.34 + or -.08 with surface roughness characterized by a standard deviation of surface slopes of 18 deg + or - 2 deg. A comparison of these results with previously published values at other wavelengths suggests that the effective lunar dielectric constant decreases with decreasing wavelength.
White, T. L.↗
Atmospheric absorption measurements in the region of 1 mm wavelength.
A Froome-type plasma-metal-junction device (1962) was used in high-resolution radiation transmission measurements in the atmosphere at wavelengths from 0.5 to 3.0 mm. The experimental and theoretical results for water vapor absorption lines in two submillimeter wavelength windows were compared, showing that this technique provided a much higher wavelength accuracy than more conventional optical-type spectroscopy.
Emery, R.↗
Observations of the total lunar eclipse on February 10, 1971 at 3.1 mm wavelength.
Observations were made of the total lunar eclipse on February 10, 1971 at a wavelength of 3.1 mm at the Millimeter Wave Observatory of the University of Texas at Austin. Eclipse cooling curves obtained for Copernicus, Mare Serenitatis, and a mountainous region indicate maximum temperature decreases of 6.77%, 6.37%, and 7.51%, respectively. Cooling rates of about 6 K/hour were measured. The normalized solar insolation has also been calculated for each region.
Ulich, B. L.↗
Parametric study of the lubrication of thrust loaded 120-mm bore ball bearings to 3 million DN
A parametric study was performed with 120-mm bore angular-contact ball bearings under varying thrust loads, bearing and lubricant temperatures, and cooling and lubricant flow rates. Contact angles were nominally 20 and 24 deg with bearing speeds to 3 million DN. Endurance tests were run at 3 million DN and a temperature of 492 K (425 F) with 10 bearings having a nominal 24 deg contact angle at a thrust load of 22241 N (5000 lb). Bearing operating temperature, differences in temperatures between the inner and outer races, and bearing power consumption can be tuned to any desirable operating requirement by varying 4 parameters. These parameters are outer-race cooling, inner-race cooling, lubricant flow to the inner race, and oil inlet temperature. Preliminary endurance tests at 3 million DN and 492 K (425 F) indicate that long term bearing operation can be achieved with a high degree of reliability.
Signer, H.↗
Wind tunnel investigation of aerodynamic characteristics of a scale model of a D5 bulldozer and an M109 self-propelled 155 mm Howitzer
Wind tunnel tests were conducted on a scale model of a D5 bulldozer and an M109 self-propelled 155 MM howitzer to determine the aerodynamic characteristics of these typical externally-suspended heavy lift helicopter cargo configurations. Tests were made over a large range of pitch and yaw attitudes at a nominal Reynolds number per unit length of 1.5 x 10 to the 6th power.
Laub, G. H.↗
Lunar polarization studies at 3.1 mm wavelength
Observations of the distribution of linearly polarized lunar thermal emission were made at a wavelength of 3.1 mm with The University of Texas 4.88 m parabolic reflector (0.042 deg HPBW). A shadow corrected, rough surface, thermal emission model for a homogeneous moon was least-squares-fitted to the polarization data. Results indicate an effective lunar dielectric constant of 1.34 plus or minus 0.04 with surface roughness characterized by a standard deviation of 17 (plus or minus 5) deg for surface slopes with a normal probability density, independent of lunar phase. A comparison of these results with published values at other wavelengths suggests that the effective lunar dielectric constant, as obtained by lunar emission measurements, decreases with decreasing wavelength of observation. This wavelength dependence may be interpreted in terms of an inhomogeneous surface and/or a surface that possesses intermediate scale surface roughness.
White, T. L.↗
Early lunar history - Ages of 2 to 4 mm soil fragments from the lunar highlands
The ages of twenty-one 2 to 4 mm soil fragments from Apollo 16 stations 6, 8, 11, and 13, including all six major petrographic rock types found among Apollo 16 samples, were determined using the Ar-40/Ar-39 stepwise-heating technique. Twelve of the twenty-one samples have ages within 3.95 to 4.06 billion years, and it is believed that they represent the age of at least one stage of the Cayley Formation. Four samples have ages distinctly older than 4.00 billion years, making them the oldest lunar material found to date.
Schaeffer, O. A.↗