Radar reflectivity of Titan

Details Radar reflectivity of Titan Radar reflectivity of Titan

May 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990sci...248..975m&link_type=abstract

Science (ISSN 0036-8075), vol. 248, May 25, 1990, p. 975-980.

Astronomy and Astrophysics

Astronomy

79

Brightness Temperature, Radar Astronomy, Satellite Atmospheres, Titan, Dielectrics, Ethane, Hydrocarbons, Methane, Microwave Reflectometers, Planetary Surfaces, Very Large Array (Vla), Saturn, Satellites, Titan, Radar Methods, Reflectivity, Wavelengths, Microwaves, Earth-Based Observations, Astronomy, Atmosphere, Ethane, Composition, Hydrocarbons, Emissions, Scattering, Brightness Temperature, Surface, Diagrams, Geometry, Equipment, Procedure, Interferometry, Spectra, Amplitude, Thermal Emissions, Structure

Scientific paper

The low dielectric constant of the liquid hydrocarbon and ethane-methane surface mixture of Titan has as a direct consequence a set of unique microwave-reflection properties which were sought out at 3.5-cm wavelength, using a 70-m transmitting antenna in conjunction with the VLA as a receiving instrument. The statistically significant echoes obtained indicate that Titan is not covered with a deep global ocean of ethane. A global ocean as shallow as about 200 m would have exhibited reflectivities smaller by an order of magnitude, and below the experiment's detection limit.

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