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Multicolor photoelectric photometry of the brighter planets. I.
Multicolor photoelectric photometry of brighter planets and moon emphasizing algorithm for determining atmospheric extinction
Detailed photoelectric photometry of the moon.
Photoelectrically determined photometric function of Moon correlated with color, normal albedo and geomorphology
Two-color photoelectric photometry of the earth-shine.
Two-color photoelectric photometry of earthshine, determining earth albedos
Multicolor photoelectric photometry of Uranus
Narrow band and UBV photoelectric photometry of Uranus geometric albedo and magnitude at unit distance as functions of wavelength
An attempt to define luminosity criteria in O stars via narrow-band photoelectric photometry
Luminosity criteria in O stars via narrow band photoelectric photometry suggesting VI Cygni proximity
Multicolor photoelectric photometry of the brighter planets. III - Observations from Boyden Observatory.
Photoelectric photometry of Mercury, Venus, Mars, Jupiter and Saturn /1963-1965/, determining phase curves and monochromatic albedos
Photoelectric photometry of Comet P/Halley from Mauna Kea Observatory
A program of photoelectric photometry of comet Halley yielded 60 nights of usable photometry. The uncertainty in the photometry in all filters except OH is better than 2%. Throughout the apparition, the comet is brightest in the filters that isolated the neutral gas emission features of OH, CN, C2, and C3. The fluxes in the filters that isolated the ionic emission features of CO(+) and H2O(+) are comparable to the continuum when centered upon the optocenter, thereby making the ionic emission weak to undetectable above the continuum. The continuum colors do not appear to be a function of phase angle; therefore, the colors are probably indicative of dust grain composition and are not dominated by scattering geometry effects.
Multicolor photoelectric photometry of the brighter planets. II - Observations from Le Houga Observatory.
Multicolor photoelectric photometry of Venus, Mars, Jupiter and Saturn, noting phase curves and monochromatic geometric albedos of Mars and Jupiter
Multicolor photoelectric photometry of Neptune.
Mean opposition magnitudes at unit distance and geometric albedos obtained as functions of wavelength from multicolor photoelectric photometry observations of Neptune performed in southern France and South Africa are presented. The measurements were made in the standard UBV bands and in seven narrow bands isolated by interference filters between 0.314 and 0.627 microns.
Study of lunar earthshine by photoelectric photometry Semiannual report, 1 Nov. 1965 - 30 Apr. 1966
Photoelectric photometer developed to measure earth albedo and lunar earthshine
Rotation of Comet P/Tempel 2 from CCD and photoelectric photometry
Two lightcurves have been obtained of the periodic comet Tempel 2 during May and June 1988, using a CCD camera, as well as five photoelastic photometer lightcurves. On each observational occasion, two uneven maxima were observed which suggest that the lightcurves in question are not products of an active spot on the comet, but rather are true reflections from an elongated rotating nucleus that are being observed through a transparent coma. A comparison of CCD and photoelectric photometry leads to an encouragement of users of the latter to sustain their efforts with such instruments.
Five-color photoelectric photometry of asteroid 433 Eros
Five-color (UVBGR) photoelectric light curves of Eros are presented which were obtained on nine nights during the asteroid's 1974/75 close apparition. Indications that three reversals occurred in the relative depths of the two minima between late December 1974 and late January 1975 are noted along with definite evidence of phase reddening. The maximum amplitude observed was 1.44 magnitudes, and the absolute visual magnitude at primary maximum (corrected to zero phase and to 1 AU from the earth and the sun) was about 10.8 magnitudes. Since the observations indicate that Eros has no significant rotational color variations, it is suggested that the light-curve amplitudes are due primarily to the asteroid's shape and to shadowing effects. Based on its colors relative to the sun, it is concluded that Eros appears to be an S-type asteroid.
Analysis of Mount St. Helens ash from optical photoelectric photometry
The optical properties of suspended dust particles from the eruption of Mt. St. Helens on July 23, 1980 are investigated using photoelectric observations of standard stars obtained on the 0.76-m telescope at the University of Washington 48 hours after the eruption. Measurements were made with five broad-band filters centered at 3910, 5085, 5480, 6330, and 8050 A on stars of varying color and over a wide range of air masses. Anomalous extinction effects due to the volcanic ash were detected, and a significant change in the wavelength-dependent extinction parameter during the course of the observations was established by statistical analysis. Mean particle size (a) and column density (N) are estimated using the Mie theory, assuming a log-normal particle-size distribution: a = 0.18 micron throughout; N = 1.02 x 10 to the 9th/sq cm before 7:00 UT and 2.33 x 10 to the 9th/sq cm after 8:30 UT on July 25, 1980. The extinction is attributed to low-level, slowly migrating ash, possibly combined with products of gas-to-particle conversion and coagulation.
Study of lunar earthshine by photoelectric photometry Final report, 1 Nov. 1965 - 30 Sep. 1967
Design feasibility and performance of semiportable field instrument for monitoring changes in earth albedo via earthshine measurements
Multicolor photoelectric photometry of the Moon, Venus, Mars, and other planets Final report, 15 Jun. 1960 - 31 Jan. 1968
Multicolor electrophotometry of brighter planets
Photoelectric photometry of HD 116994.
HD 116994 period, discussing harmonic analyses made of light and color curves, visual magnitude estimation, pulsation theory results and observation result tables
Preliminary results of OAO ultraviolet photoelectric photometry of galaxies
General results are presented based on nearly completed reductions of data for approximately 35 galaxies of all Hubble types. In general the visual and ultraviolet energy distributions are well correlated. The energy distribution in late-type galaxies appears to turn up sharply in the region around 2000 A, and this is tentatively interpreted as due to the presence of early-type stars whose energy distribution is modified by interstellar dust within these objects. Similar turnups may be present in several elliptical galaxies but the evidence at this time is not definitive.