author={K. Baines and P. Drossart and T. Momary and V. Formisano and C. Griffith and G. Bellucci and J. Bibring and R. Brown and B. Buratti and F. Capaccioni and P. Cerroni and R. Clark and A. Coradini and M. Combes and D. Cruikshank and R. Jaumann and Y. Langevin and D. Matson and T. McCord and V. Mennella and R. Nelson and P. Nicholson and B. Sicardy and C. Sotin},
  journal={Earth, Moon, and Planets},
AbstractThe wide spectral coverage and extensive spatial, temporal, and phase-angle mapping capabilities of the Visual Infrared Mapping Spectrometer (VIMS) onboard the Cassini-Huygens Orbiter are producing fundamental new insights into the nature of the atmospheres of Saturn and Titan. For both bodies, VIMS maps over time and solar phase angles provide information for a multitude of atmospheric constituents and aerosol layers, providing new insights into atmospheric structure and dynamical and… Expand
On the Discovery of CO Nighttime Emissions on Titan by Cassini/VIMS: Derived Stratospheric Abundances and Geological Implications
Abstract We present a quantitative analysis of CO thermal emissions discovered on the nightside of Titan by Baines et al. [2005. The atmospheres of Saturn and Titan in the near-infrared: FirstExpand
The three-dimensional structure of Saturn's equatorial jet at cloud level
Abstract The three-dimensional structure of Saturn's intense equatorial jet from latitudes 8° N to 20° S is revealed from detailed measurements of the motions and spectral reflectivity of clouds atExpand
Saturn's tropospheric composition and clouds from Cassini/VIMS 4.6-5.1μm nightside spectroscopy
Abstract The latitudinal variation of Saturn’s tropospheric composition (NH 3 , PH 3 and AsH 3 ) and aerosol properties (cloud altitudes and opacities) are derived from Cassini/VIMS 4.6–5.1 μmExpand
The abundances of constituents of Titan's atmosphere from the GCMS instrument on the Huygens probe
Direct atmospheric measurements from the Gas Chromatograph Mass Spectrometer (GCMS), including altitude profiles of the constituents, isotopic ratios and trace species (including organic compounds), were reported, confirming the primary constituents were confirmed to be nitrogen and methane. Expand
Modeling transmission windows in Titan’s lower troposphere: Implications for infrared spectrometers aboard future aerial and surface missions
Abstract From orbit, the visibility of Titan’s surface is limited to a handful of narrow spectral windows in the near-infrared (near-IR), primarily from the absorption of methane gas. This hasExpand
Titan solar occultation observed by Cassini/VIMS: Gas absorption and constraints on aerosol composition
Abstract A solar occultation by Titan's atmosphere has been observed through the solar port of the Cassini /VIMS instrument on January 15th, 2006. Transmission spectra acquired during solar egressExpand
Chapter 7 Clouds and Aerosols in Saturn ’ s Atmosphere
In this chapter we review the photochemical and thermochemical equilibrium theories for the formation of condensate clouds and photochemical haze in Saturn’s upper troposphere and stratosphere andExpand
A review of Titan’s atmospheric phenomena
Saturn’s satellite Titan is a particularly interesting body in our solar system. It is the only satellite with a dense atmosphere, which is primarily made of nitrogen and methane. It harbours anExpand
The Transit Transmission Spectrum of a Cold Gas Giant Planet
We use solar occultations observed by the Visual and Infrared Mapping Spectrometer aboard the Cassini Spacecraft to extract the 1 to 5 micron transmission spectrum of Saturn, as if it were aExpand
Titan’s cloud seasonal activity from winter to spring with Cassini/VIMS
Abstract Since Saturn orbital insertion in July 2004, the Cassini orbiter has been observing Titan throughout most of the northern winter season (October 2002–August 2009) and the beginning ofExpand


Release of volatiles from a possible cryovolcano from near-infrared imaging of Titan
Near-infrared images of Titan obtained on 26 October 2004 by the Cassini spacecraft show that a widespread methane ocean does not exist; subtle albedo variations instead suggest topographical variations, as would be expected for a more solid (perhaps icy) surface. Expand
The Cassini Visual And Infrared Mapping Spectrometer (Vims) Investigation
The Cassini visual and infrared mapping spectrometer (VIMS) investigation is a multidisciplinary study of the Saturnian system. Visual and near-infrared imaging spectroscopy and high-speedExpand
A New Look at the Saturn System: The Voyager 2 Images
Within Saturn's rings, the "birth" of a spoke has been observed, and surprising azimuthal and time variability is found in the ringlet structure of the outer B ring, leading to speculations about Saturn's internal structure and about the collisional and thermal history of the rings and satellites. Expand
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. Expand
Titan’s 5-μm window: observations with the Very Large Telescope
Abstract We report on mid-resolution ( R ∼2000) spectroscopic observations of Titan, acquired in November 2000 with the Very Large Telescope and covering the range 4.75–5.07 μm. These observationsExpand
A physical model of Titan's aerosols.
Microphysical simulations of Titan's stratospheric haze show that aerosol microphysics is linked to organized dynamical processes, and the aerosol's electrical charge is critical for the particle size and optical depth of the haze. Expand
Titan's Atmospheric Temperatures, Winds, and Composition
Early Cassini infrared observations of Titan show a stratopause at an altitude of 310 kilometers (and 186 kelvin at 15°S), and the concentrations of several stratospheric organic compounds are enhanced at mid- and high northern latitudes, and the strong zonal winds may inhibit mixing between these latitudes and the rest of Titan. Expand
Discrete cloud activity in Saturn’s equator during 1995, 1996 and 1997
Abstract A regular extensive CCD imaging of Saturn allowed us to analyze the discrete cloud activity in the Equatorial Zone from 1995 to 1997. The large-scale storm observed in 1994 at +10° (Expand
Titan's 5-micron lightcurve
Abstract We report on repeated mid-resolution (R∼2000) spectroscopic observations of Titan, acquired between November 2002 and January 2003 with ISAAC at the ESO/VLT and covering the 4.84–5.05 μmExpand
Temperatures, Winds, and Composition in the Saturnian System
Diurnal surface temperature variations on Phoebe suggest a more porous regolith than on the jovian satellites, and Saturn's ring temperatures have radial variations down to the smallest scale resolved (100 kilometers). Expand