V photometry of Titania, Oberon, and Triton

Details V photometry of Titania, Oberon, and Triton V photometry of Titania, Oberon, and Triton

Feb 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989icar...77..239g&link_type=abstract

Icarus (ISSN 0019-1035), vol. 77, Feb. 1989, pt. 1, p. 239-247.

Astronomy and Astrophysics

Astronomy

45

Astronomical Photometry, Oberon, Planetary Orbits, Titania, Triton, Albedo, Asteroids, Brightness, Regolith, Planets, Satellites, Uranus, Neptune, Photometry, Titania, Oberon, Triton, Earth-Based Observations, Brightness, Surface, Lightcurves, Telescope Methods, Rotation, Albedo, Voyager 2 Mission, Magnitude, Data, Spacecraft Observations, Wavelengths, Photometry, Comparisons, Regolith, Atmosphere, Optical Properties

Scientific paper

The phase angle and orbital brightness variations of Titania, Oberon, and Triton are presently obtained through analysis of V filter photometry obtained at Mauna Kea in 1982-1983. While Titania and Oberon exhibit magnitude variations with phase angle comparable to those of low-to-moderate albedo asteroids observed within several deg of opposition, Triton's phase variation is distinctly different from these and has a phase coefficient consistent with either a high-albedo regolith or an optically thick nonparticulate scattering layer (perhaps an atmosphere, or an ocean). A low-albedo regolith cannot on the strength of these data be ruled out, however.

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