Methane rain on Titan

Journal Article · Mon Aug 01 00:00:00 EDT 1988 · Icarus; (United States)

DOI:https://doi.org/10.1016/0019-1035(88)90005-X· OSTI ID:6740515

Toon, O B; Mckay, C P; Courtin, R; Ackerman, T P

The atmosphere of Titan is characterized by means of model computations based on Voyager IRIS IR spectra and published data from laboratory determinations of absorption coefficients and cloud refractive indices. The results are presented in tables and graphs, and it is pointed out that the presence of Ar is not required in the model. Particular attention is given to the role of CH4, which is found to form patchy clouds (with particle radii of 50 microns or greater and visible/IR optical depths of 2-5) at altitudes up to about 30 km. The mechanisms by which such rain-sized particles could form are discussed, and it is suggested that the observed 500-600/cm spectrum is affected much less by the CH4 clouds than by H2 or variations in the temperature of the high-altitude haze. 42 references.

• Research Organization: NASA, Ames Research Center, Moffett Field, CA (USA)
• OSTI ID: 6740515
• Journal Information: Icarus; (United States), Vol. 75
• Country of Publication: United States
• Language: English

Related Subjects

71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
SATURN PLANET
SATELLITE ATMOSPHERES
ABSORPTIVITY
CHEMICAL COMPOSITION
INFRARED RADIATION
MATHEMATICAL MODELS
METHANE
OPTICAL PROPERTIES
RAIN
REFRACTIVITY
VOYAGER SPACE PROBES
ALKANES
ATMOSPHERES
ATMOSPHERIC PRECIPITATIONS
ELECTROMAGNETIC RADIATION
HYDROCARBONS
ORGANIC COMPOUNDS
PHYSICAL PROPERTIES
PLANETS
RADIATIONS
SPACE VEHICLES
VEHICLES
640107* - Astrophysics & Cosmology- Planetary Phenomena