Engineering topics
Publications and source records attributed to Ney, E. P..
Photometric measurements from 2.2 to 18 microns are reported for six southern RV Tauri stars. Four of the six have anomalous infrared excess radiation similar to that observed in other RV Tauri stars. The infrared spectra of IW Car, AR Pup, and SX Cen resemble that of oxygen-rich RV Tau. RU Cen is similar to AC Her.
The brightness and polarization of the zodiacal light have been measured from the satellite OSO-5, using two photometers of effective wavelengths 4180 and 6820 A. The satellite configuration restricts the observations to ecliptic longitudes close to 90 deg, but measurements have been made from the ecliptic to the poles. On the ecliptic, the intensity of the zodiacal light was found to be 117 S10 (blue) and 315 S10 (red) with polarizations of 16.5 and 15 per cent, respectively. At the ecliptic poles the zodiacal intensity was 35 S10 (blue) with 20 per cent polarization. No temporal changes in zodiacal light have been found nor any significant differences in the intensities in the two hemispheres. The direction of polarization of the zodiacal light has been shown to be H-pass radial.
Polarization measurements made from the satellite OSO-5 show that the polarized intensity in the direction of the Scutum arm of the Galaxy is different in intensity and direction of the polarization from that observed due to the zodiacal light. The observations are consistent with polarized diffuse galactic light superposed on the zodiacal light. The results are interpreted in terms of a model in which the galactic starlight is scattered by interstellar dust.
Spectroscopic study of 30 Southern-Hemisphere M supergiants mostly in Carina in the blue and near-infrared, and photometrical study of these stars from 0.4 to 18 microns. The uncertainties in the determinations of interstellar extinction are discussed, and the spatial distribution of the M supergiants in the Carina arm is shown. The presence of the 11-micron excess attributed to silicate dust is a common feature. Stars of the same spectral type and luminosity class are remarkably homogeneous in their long-wave behavior. The silicate feature becomes more prominent in the more luminous stars and in stars of later spectral type. Four composite systems show little long-wave excess. The two VV Cephei objects have excesses probably produced by gas emission, and the other two have little or no excess - supporting the suggestion that the presence of the early star prohibits the formation of a dust envelope. Three stars - VY CMa, VX Sgr, and HD 9767 - appear to be extreme examples of stars with large excesses over the entire long-wave region. It is suggested that these objects are surrounded by large amounts of particulate material over a great range of distances from the stars.
Infrared radiation from the nucleus of NGC 5128 has been measured from 1 to 10 microns. Scans and aperture-size data show that there is only one bright infrared region within the central 1 min of the galaxy and that it is coincident to within 5 sec with the ?hot spot' of Kunkel and Bradt. The 3.5- and 2.2-micron radiation is more peaked toward the center than are the shorter wavelengths. The data are interpreted to indicate a small nonstellar infrared core superposed on an extended, reddened stellar component.
Observations made during the Gemini 5, 9, and 10 missions in the context of their relation to ground-based and balloon-based experiments on dim-light phenomena are reported. Zodiacal light is the visible manifestation of dust grains in orbit around the sun. The negatives that were exposed on the Gemini 9 mission were studied by the use of an isodensitracer to produce intensity isophotes. Data on the following factors were obtained: (1) intensity distribution of the zodiacal light, both morning and evening; (2) the height and intensity of the airglow at various geographic positions; and (3) intensity distribution of the Milky Way in the region of the sky near Cygnus. Also, a previously unreported phenomenon was discovered. This phenomenon appeared as an upward extension of the normal 90-kilometer airglow layer. The extension was in the form of wisps or plumes approximately 5 deg wide and extending upward approximately 5 deg. The results obtained from pictures exposed on the Gemini 10 mission were of qualitative or geometrical value only.
During Gemini missions, the image orthicon system was used to obtain photographic data on faint and diffuse astronomical phenomena. Results show that the photographs may be used to determine the airglow geometry. Although it was sensitive, the original photographic system was unsuitable for use in the study of dim and diffuse astronomical light sources.
Lightning observation by OSO-E satellite, suggesting maximum thunderstorm incidence over North Atlantic Ocean
High luminosity G supergiants at 0.4-18 micron wavelengths showing intense silicate emission shell
Mercury planet average dark side temperature indicating top surface layer similarity with moon
F region night airglow in equatorial and midlatitudes, discussing red and blue emission origins
Ic class variables long wavelength anomalous radiation, discussing emission from circumstellar dust shell
Nighttime lightning activity observations by orbiting solar satellite OSO-B, determining thunderstorms positions by optical radiation detection
Comet Bennett 1969i photometric observations, showing blackbody-like continuum at short wavelengths with sharp peak due to silicate grains
Lunar thermal anomalies in various craters observed during lunar night by IR methods, with data suggesting hot and cold regions
Broadband photometry for circumstellar IR emission from cool stars, considering giant and carbon stars
Double structure in IR near Trapezium region of M42 in Orion Nebula center
OSO-B2 satellite zodiacal light observations at constant 90 degree elongation, measuring polarized component as function of time