Release of volatiles from a possible cryovolcano from near-infrared imaging of Titan

  title={Release of volatiles from a possible cryovolcano from near-infrared imaging of Titan},
  author={Christophe Sotin and Ralf Jaumann and Bonnie J. Buratti and R. Hamilton Brown and Roger N. Clark and Laurence A. Soderblom and Kevin H. Baines and Giancarlo Bellucci and J. P. Bibring and Fabrizio Capaccioni and Priscilla Cerroni and Michel Combes and Angioletta Coradini and Dale P. Cruikshank and Pierre Drossart and Vittorio Formisano and Y. Langevin and Dennis Matson and Thomas B. McCord and Robert M. Nelson and Philip D. Nicholson and Bruno Sicardy and S. Lemou{\'e}lic and S{\'e}bastien Rodriguez and Katrin Stephan and C. K. Scholz},
Titan is the only satellite in our Solar System with a dense atmosphere. The surface pressure is 1.5 bar (ref. 1) and, similar to the Earth, N2 is the main component of the atmosphere. Methane is the second most important component, but it is photodissociated on a timescale of 107 years (ref. 3). This short timescale has led to the suggestion that Titan may possess a surface or subsurface reservoir of hydrocarbons to replenish the atmosphere. Here we report near-infrared images of Titan… 

Sequestration of Ethane in the Cryovolcanic Subsurface of Titan

Saturn’s largest satellite, Titan, has a thick atmosphere dominated by nitrogen and methane. The dense orange-brown smog hiding the satellite’s surface is produced by photochemical reactions of

Titan: an astrobiological laboratory in the solar system

After only three years of close observation from the Cassini-Huygens mission, Titan appears more and more as one of the key planetary bodies in the solar system for astrobiological studies. Titans

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.

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

T The Exploration of Titan

INTRODUCTION The most Earth-like body in the solar system is not another planet but Saturn’s largest moon, Titan.1 Indeed, if Titan orbited the Sun rather than Saturn, we would not hesitate to call

Astrobiology of Titan

Mars, Europa, and Titan—these solar system bodies have a great exobiological significance. Here, we will focus on Titan, the largest satellite of Saturn, which has a dense atmosphere composed

Astrobiology and habitability of Titan

Largest satellite of Saturn and the only in the solar system having a dense atmosphere, Titan is one of the key planetary bodies for astrobiological studies, due to several aspects. (i) Its analogies

Methane drizzle on Titan

It is shown that the in situ data on the methane concentration and temperature profile in Titan's troposphere point to the presence of layered optically thin stratiform clouds, indicating that methane precipitation occurs wherever there is slow upward motion.

Evolution of Titan and implications for its hydrocarbon cycle

  • G. TobieM. Choukroun L. Le Corre
  • Geology
    Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences
  • 2008
Measurements of the carbon and nitrogen isotopic ratios as well as the detection of 40Ar and 36Ar by the gas chromatograph mass spectrometer (GCMS) instrument on board the Huygens probe have provided



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

Photochemistry of the atmosphere of Titan: comparison between model and observations.

The photochemistry of simple molecules containing carbon, hydrogen, nitrogen, and oxygen atoms in the atmosphere of Titan has been investigated using updated chemical schemes and the authors' own estimates of a number of key rate coefficients, which satisfactorily accounts for the concentrations of minor species observed by the Voyager IRIS and UVS instruments.

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.

Europa: Tidal heating of upwelling thermal plumes and the origin of lenticulae and chaos melting

Tidal heating models are linked to thermal convection models for ice having strongly temperature dependent viscosity. In the range of ice viscosity inferred from laboratory experiments, tidal forces

Titan: a Satellite with an Atmosphere.

The Surface of Titan from NICMOS Observations with the Hubble Space Telescope

Abstract From diffraction-limited images produced by the near-IR camera NICMOS aboard the Hubble Space Telescope we derived maps of Titan's surface in the methane windows near 1.1, 1.6, and 2.0 μm.

Atmospheric models of Titan and Triton