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Article is made available in accordance with the publisher's policy and may be subject to US copyright law. Please refer to the publisher's site for terms of use. The MIT Faculty has made this article openly available. Please share how this access benefits you. Your story matters. ABSTRACT Cassini/VIMS T85 observations of a solar specular reflection off of(More)
Clouds on Titan result from the condensation of methane and ethane and, as on other planets, are primarily structured by circulation of the atmosphere. At present, cloud activity mainly occurs in the southern (summer) hemisphere, arising near the pole and at mid-latitudes from cumulus updrafts triggered by surface heating and/or local methane sources, and(More)
We describe a mission concept for a stand-alone Titan airplane mission: Aerial Vehicle for In-situ and Airborne Titan Reconnaissance (AVI-ATR). With independent delivery and direct-to-Earth communications, AVI-ATR could contribute to Titan science either alone or as part of a sustained Titan Exploration Program. As a focused mission, AVIATR as we have(More)
Cassini/VIMS high-phase specular observations of Titan's north pole during the T85 flyby show evidence for isolated patches of rough liquid surface within the boundaries of the sea Punga Mare. The roughness shows typical slopes of 6° ± 1°. These rough areas could be either wet mudflats or a wavy sea. Because of their large areal extent, patchy geographic(More)
Only a few impact craters have been unambiguously detected on Titan by the Cassini-Huygens mission. Among these, Sinlap is the only one that has been observed both by the RADAR and VIMS instruments. This paper describes observations at centimeter and infrared wavelengths which provide complementary information about the composition, topography, and 45(More)
The surface of Titan, the largest icy moon of Saturn, is veiled by a very thick and hazy atmosphere. The Visual and Infrared Mapping Spectrometer onboard the Cassini spacecraft, in orbit around Saturn since July 2004, conduct an intensive survey of Titan with the objective to understand the complex nature of the atmosphere and surface of the mysterious moon(More)
1 In this paper, we characterize the morphology of the disk-integrated phase 2 functions of satellites and rings around the giant planets of our Solar Sys-3 tem. We find that the shape of the phase function is accurately represented 4 by a logarithmic model (Bobrov, 1970, in Surfaces and Interiors of Planets 5 and Satellites, Academic, edited by A.(More)
Revised ———– (date) ABSTRACT Simulations of Titan's atmospheric transmission and surface reflectivity have been developed in order to estimate how Titan's atmosphere and surface properties could affect performances of the Cassini radar experiment. In this paper we present a selection of models for Titan's haze, vertical rain distribution, and surface(More)
The MIT Faculty has made this article openly available. Please share how this access benefits you. Your story matters. Abstract Observations from Cassini VIMS and ISS show localized but extensive surface brightenings in the wake of the 2010 September cloudburst. Four separate areas, all at similar latitude, show similar changes: Yalaing Terra, Hetpet Regio,(More)
Titan is the largest satellite of Saturn, and the only one to have a dense atmosphere. Whereas its surface cannot be seen at visible wavelengths due to the strong absorption and scattering of the atmospheric gases (mainly N<inf>2</inf> and CH<inf>4</inf>) and aerosols, it can be seen at specific wavelengths in the infrared. We focus in this paper on the(More)