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Title: V photometry of Titania, Oberon, and Triton

Abstract

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. 39 references.

Authors:
; ;
Publication Date:
Research Org.:
California Institute of Technology, Pasadena (USA); Hawaii Univ., Honolulu (USA)
OSTI Identifier:
5763026
Resource Type:
Journal Article
Resource Relation:
Journal Name: Icarus; (United States); Journal Volume: 77
Country of Publication:
United States
Language:
English
Subject:
71 CLASSICAL AND QUANTUM MECHANICS, GENERAL PHYSICS; NEPTUNE PLANET; SATELLITES; PHOTOMETRY; SATURN PLANET; URANUS PLANET; ALBEDO; BRIGHTNESS; ORBITS; OVERBURDEN; SATELLITE ATMOSPHERES; VARIATIONS; ATMOSPHERES; OPTICAL PROPERTIES; PHYSICAL PROPERTIES; PLANETS; 640107* - Astrophysics & Cosmology- Planetary Phenomena

Citation Formats

Goguen, J.D., Hammel, H.B., and Brown, R.H. V photometry of Titania, Oberon, and Triton. United States: N. p., 1989. Web. doi:10.1016/0019-1035(89)90088-2.
Goguen, J.D., Hammel, H.B., & Brown, R.H. V photometry of Titania, Oberon, and Triton. United States. doi:10.1016/0019-1035(89)90088-2.
Goguen, J.D., Hammel, H.B., and Brown, R.H. 1989. "V photometry of Titania, Oberon, and Triton". United States. doi:10.1016/0019-1035(89)90088-2.
@article{osti_5763026,
title = {V photometry of Titania, Oberon, and Triton},
author = {Goguen, J.D. and Hammel, H.B. and Brown, R.H.},
abstractNote = {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. 39 references.},
doi = {10.1016/0019-1035(89)90088-2},
journal = {Icarus; (United States)},
number = ,
volume = 77,
place = {United States},
year = 1989,
month = 2
}
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