Tidal effects of disconnected hydrocarbon seas on Titan

  title={Tidal effects of disconnected hydrocarbon seas on Titan},
  author={Stanley F. Dermott and Carl E. Sagan},
THERMODYNAMIC and photochemical arguments1–4 suggest that Titan, the largest satellite of Saturn, has a deep ocean of liquid hydrocarbons. At visible wavelengths, Titan's surface is obscured by a thick stratospheric haze, but radar observations5–7 have revealed large regions of high surface reflectivity that are inconsistent with a global hydrocarbon ocean. Titan's surface has also been imaged at infrared wavelengths8–10, and the highest-resolution data (obtained by the Hubble Space Telescope… 

Wind-driven surface waves on Titan

The surface of Titan represents the largest surface area in the solar system essentially unexplored, although recent observations from Hubble Space Telescope and ground-based telescopes using

Tidal Winds on Titan Caused by Saturn

Abstract The influence of Saturn's gravitational tide on the atmosphere of Titan is investigated by means of a three-dimensional general circulation model. Titan's orbital eccentricity of 0.0292

The dynamic meteorology of Titan

Simulation of tides in hydrocarbon lakes on Saturn’s moon Titan

Numerous hydrocarbon lakes have recently been detected on Saturn’s largest moon Titan, representing the only known large bodies of liquids on a planetary surface outside the Earth. In the context of

The Throat of Kraken: Tidal Dissipation and Mixing Timescales in Titan's Largest Sea

Introduction: Of Titan’s three seas, Kraken has the largest area, and sprawls over the widest range of latitude and longitude. This extent means it sees the largest variations in tidal accelerations

Geology and surface processes on titan

The surface of Titan has been revealed globally, if incompletely, by Cassini observations at infrared and radar wavelengths as well as locally by the instruments on the Huygens probe. Extended dune

Surface of Titan revealed by Cassini/Huygens

Titan is Saturn's largest moon, and the second-largest natural satellite in the solar system. The surface is obscured from view by suspended haze layers, which are the products of methane



Evidence for surface heterogeneity on Titan

UNLIKE all other planetary satellites, Saturn's moon Titan has a massive atmosphere1–8. At visible wavelengths, a thick stratospheric haze hides the surface from view. The emission from Titan in the

Does Titan have an ocean? A review of current understanding of Titan's surface

The nature of Titan's surface has been a fascinating puzzle since the first definitive detection of an atmosphere in 1944. Pre-Voyager models of the surface based largely on cosmochemistry and the

The tide in the seas of Titan

The surface temperature of Titan1 is about 95 K, between the melting point (90.6 K) and the boiling point (118 K) of methane at the total surface pressure of 1.6 bar. Voyager 1 IR observations1,2

Encounter with saturn: voyager 1 imaging science results.

As Voyager 1 flew through the Saturn system it returned photographs revealing many new and surprising characteristics of this complicated community of bodies, including small inner satellites that interact gravitationally with one another and with the ring particles in ways not observed elsewhere in the solar system.

Oceans on Titan?

If global oceans of methane exist on Titan, the atmosphere above them must be within 2 percent of saturation, since the two Voyager radio occultation soundings probably occurred over land.

Ethane Ocean on Titan

It is proposed that Saturn's satellite Titan is covered by an ocean one to several kilometers deep consisting mainly of ethane, and the coexisting atmosphere is compatible with Voyager data.

Tides and tidal energy

Abstract The present article reviews our understanding of the tides and of the flow of tidal energy through the oceans. The residence time for tidal energy in the oceans is short, and this results in

Titan's Rotation: Surface Feature Observed

Abstract We have detected time variation in Titan's geometric albedo in methane windows at 0.94, 1.08, and 1.28 μm, relative to its albedo in adjacent methane bands, of 8 ± 5%, 14 ± 3%, and 22 ± 3%,