Size and Shape of Saturn's Moon Titan

  title={Size and Shape of Saturn's Moon Titan},
  author={Howard A. Zebker and Bryan W. Stiles and Scott Hensley and Ralph D. Lorenz and Randolph L. Kirk and Jonathan I. Lunine},
  pages={921 - 923}
Global Analysis of Titan In its orbit around Saturn, the Cassini spacecraft passes regularly by the planet's largest moon, Titan. Using a radar instrument to peer through the moon's thick atmosphere, Zebker et al. (p. 921, published online 2 April) developed a global model of Titan. Titan is slightly oblate, so that its poles have lower elevations than the equator, which may explain why the moon's hydrocarbon lakes are located at high latitudes. Titan’s poles lie at lower elevations than the… 
Gravity Field, Shape, and Moment of Inertia of Titan
Gravity data from four flybys of the Cassini spacecraft past Saturn's moon, Titan, is used to model the moon's gravity field and probe its deep interior structure, implying that Titan is a partially differentiated body with a core consisting of a mix of ice and rock or hydrated silicates.
Revealing Titan's Interior
  • F. Sohl
  • Geology, Physics
  • 2010
Evidence based on the analysis of its gravitational field that the interior of Titan was much colder than previously thought, and thereby impeded substantial melting and subsequent separation of the primordial ice-rock mixture is reported.
New clues on the interior of Titan from its rotation state
Abstract The Saturnian satellite Titan is one of the main targets of the Cassini-Huygens mission, which revealed in particular Titan's shape, gravity field, and rotation state. The shape and gravity
Titan and habitable planets around M-dwarfs.
  • J. Lunine
  • Geology, Physics
    Faraday discussions
  • 2010
The Cassini-Huygens mission discovered an active "hydrologic cycle" on Saturn's giant moon Titan, in which methane takes the place of water, meaning that in any particular planetary system, a body like Titan will always be outside the orbit of an Earth-type planet.
Titan as Revealed by the Cassini Radar
Titan was a mostly unknown world prior to the Cassini spacecraft’s arrival in July 2004. We review the major scientific advances made by Cassini’s Titan Radar Mapper (RADAR) during 13 years of
Structural and tidal models of Titan and inferences on cryovolcanism
Titan, Saturn's largest satellite, is subject to solid body tides exerted by Saturn on the timescale of its orbital period. The tide‐induced internal redistribution of mass results in tidal stress
Titan's surface geology
2.1 Overview The presence of an atmosphere, initially suggested based on limb darkening by Sola (1904) and later by the presence of methane spectral lines by Kuiper (1944), has long given Titan a
New insights on Titan's interior from its obliquity
We constructed a 6-degrees of freedom rotational model of Titan as a 3-layer body consisting of a rigid core, a fluid global ocean, and a floating ice shell. The ice shell exhibits
Titan's Interior Structure
The goal of this chapter is to give a description of Titan's interior that is consistent with the new constraints provided by the Cassini mission. As the Cassini mission proceeds into its first


Imaging of Titan from the Cassini spacecraft
Observations of Titan from the imaging science experiment onboard the Cassini spacecraft reveal intricate surface albedo features that suggest aeolian, tectonic and fluvial processes, and imply that substantial surface modification has occurred over Titan's history.
The lakes of Titan
These northern-hemisphere lakes constitute the strongest evidence yet that a condensable-liquid hydrological cycle is active in Titan’s surface and atmosphere, in which the lakes are filled through rainfall and/or intersection with the subsurface ‘liquid methane’ table.
Origin of the orbital architecture of the giant planets of the Solar System
This model reproduces all the important characteristics of the giant planets' orbits, namely their final semimajor axes, eccentricities and mutual inclinations, provided that Jupiter and Saturn crossed their 1:2 orbital resonance.
Cassini Titan Radar Mapper
The Cassini Titan Radar Mapper is a multimode radar instrument designed to probe the optically inaccessible surface of Titan, Saturn's largest moon. The instrument is to be included in the payload of
Cassini Radar Views the Surface of Titan
The Cassini Titan Radar Mapper imaged about 1% of Titan's surface at a resolution of ∼0.5 kilometer, and larger areas of the globe in lower resolution modes. The images reveal a complex surface, with
Episodic outgassing as the origin of atmospheric methane on Titan
This work shows that episodic outgassing of methane stored as clathrate hydrates within an icy shell above an ammonia-enriched water ocean is the most likely explanation for Titan's atmospheric methane, and predicts that future fly-bys should reveal the existence of both a subsurface water ocean and a rocky core, and should detect more cryovolcanic edifices.