Titan from Cassini-Huygens

Brown, R. H.; Lebreton, J. P.; Waite, J. H.

doi:10.1007/978-1-4020-9215-2

Cited by 62 publications

(15 citation statements)

References 8 publications

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“…7. The rotation models of Mimas, Enceladus, Tethys, Dione, and Iapetus have been updated in Table 2 based on the Table 24.4 values in Roatsch et al (2009a). (The Dione model is originally from Roatsch et al (2008b); the Mimas, Tethys, and Iapetus models are originally from Roatsch et al (2009b); the revised Enceladus model was not yet derived when Roatsch et al (2008a) was published.).…”

Section: Recommendationsmentioning

confidence: 99%

Report of the IAU Working Group on Cartographic Coordinates and Rotational Elements: 2009

Archinal

A’Hearn

Bowell

et al. 2010

Celest Mech Dyn Astr

330

197

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Every three years the IAU Working Group on Cartographic Coordinates and Rotational Elements revises tables giving the directions of the poles of rotation and the prime meridians of the planets, satellites, minor planets, and comets. This report takes into account the IAU Working Group for Planetary System Nomenclature (WGPSN) and the IAU Committee on Small Body Nomenclature (CSBN) definition of dwarf planets, introduces improved values for the pole and rotation rate of Mercury, returns the rotation rate of Jupiter 123 102 B. A. Archinal et al.to a previous value, introduces improved values for the rotation of five satellites of Saturn, and adds the equatorial radius of the Sun for comparison. It also adds or updates size and shape information for the Earth, Mars' satellites Deimos and Phobos, the four Galilean satellites of Jupiter, and 22 satellites of Saturn. Pole, rotation, and size information has been added for the asteroids (21) Lutetia, (511) Davida, and (2867) Šteins. Pole and rotation information has been added for (2) Pallas and (21) Lutetia. Pole and rotation and mean radius information has been added for (1) Ceres. Pole information has been updated for (4) Vesta. The high precision realization for the pole and rotation rate of the Moon is updated. Alternative orientation models for Mars, Jupiter, and Saturn are noted. The Working Group also reaffirms that once an observable feature at a defined longitude is chosen, a longitude definition origin should not change except under unusual circumstances. It is also noted that alternative coordinate systems may exist for various (e.g. dynamical) purposes, but specific cartographic coordinate system information continues to be recommended for each body. The Working Group elaborates on its purpose, and also announces its plans to occasionally provide limited updates to its recommendations via its website, in order to address community needs for some updates more often than every 3 years. Brief recommendations are also made to the general planetary community regarding the need for controlled products, and improved or consensus rotation models for Mars, Jupiter, and Saturn.

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Section: Recommendationsmentioning

confidence: 99%

Report of the IAU Working Group on Cartographic Coordinates and Rotational Elements: 2009

Archinal

A’Hearn

Bowell

et al. 2010

Celest Mech Dyn Astr

330

197

View full text Add to dashboard Cite

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“…At a mean distance of 59 Saturn radii from Saturn, Iapetus is the only regular moon in the Solar System orbiting at the largest distance from its planet. Moreover, the moon is orbiting outside Saturn's magnetosphere (which extends up to 20 Saturn's radii, Gombosi et al (2009)) thus exposing the surface to solar weathering. Iapetus' leading hemisphere surface, corresponding to the Cassini Regio (CR), appears strongly contaminated by a layer of dark organic material and carbon dioxide Filacchione et al, 2007;Cruikshank et al, 2008Cruikshank et al, , 2010Clark et al, 2012).…”

Section: Iapetusmentioning

confidence: 99%

Saturn’s icy satellites investigated by Cassini-VIMS. IV. Daytime temperature maps

Filacchione

D’Aversa

Capaccioni

et al. 2016

Icarus

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The spectral position of the 3.6 µm continuum peak measured on Cassini-VIMS I/F spectra is used as a marker to infer the temperature of the regolith particles covering the surfaces of Saturn's icy satellites. This feature is characterizing the crystalline water ice spectrum which is the dominant compositional endmember of the satellites' surfaces. Laboratory measurements indicate that the position of the 3.6 µm peak of pure water ice is temperature-dependent, shifting towards shorter wavelengths when the sample is cooled, from about 3.65 µm at T=123 K to about 3.55 µm at T=88 K. A similar method was already applied to VIMS Saturn's rings mosaics to retrieve ring particles temperature . We report here about the daytime temperature variations observed on the icy satellites as derived from three different VIMS observation types: a) a sample of 240 disk-integrated I/F observations of Saturn's regular satellites collected by VIMS during years 2004-2011 with solar phase in the 20• -40• range, corresponding to late morning-early afternoon local times. This dataset is suitable to exploit the temperature variations at hemispherical scale, resulting in average temperature T<88 K for Mimas, T<<88 K for Enceladus, T<88 K for Tethys, T=98-118 K for Dione, T=108-128 K for Rhea, T=118-128 K for Hyperion, T=128-148 K and T>168 K for Iapetus' trailing and leading hemispheres, respectively. A typical ±5 K uncertainty is associated to the temperature retrieval. On Tethys and Dione, for which observations on both leading and trailing hemispheres are available, in average daytime temperatures higher of about 10 K on the trailing * Corresponding author, email gianrico.

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“…Titan's surface can be divided into five main spectral units identified by the Cassini/VIMS instrument: bright terrain, dark equatorial dune fields or dark-brown units, blue units, 5 µm-bright units and the dark lakes (Barnes et al, 2007;Stephan et al, 2009). In the polar regions, the solid surface appears dominantly as bright terrain, lakes, and patches identified as the 5 µm-bright unit in VIMS data Sotin et al, 2012;MacKenzie et al, 2014).…”

Section: Composition Of Titan's Solid Surfacementioning

confidence: 99%

Dissolution on Titan and on Earth: Toward the age of Titan's karstic landscapes

et al. 2015

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Titan's polar surface is dotted with hundreds of lacustrine depressions. Based on the hypothesis that they are karstic in origin, we aim at determining the efficiency of surface dissolution as a landshaping process on Titan, in a comparative planetology perspective with the Earth as reference. Our approach is based on the calculation of solutional denudation rates and allow inference of formation timescales for topographic depressions developed by chemical erosion on both planetary bodies. The model depends on the solubility of solids in liquids, the density of solids and liquids, and the average annual net rainfall rates. We compute and compare the denudation rates of pure solid organics in liquid hydrocarbons and of minerals in liquid water over Titan and Earth timescales. We then investigate the denudation rates of a superficial organic layer in liquid methane over one Titan year. At this timescale, such a layer on Titan would behave like salts or carbonates on Earth depending on its composition, which means that dissolution processes would likely occur, but would be 30 times slower on Titan compared to the Earth due to the seasonality of precipitation. Assuming an average depth of 100 m for Titan's lacustrine depressions, these could have developed in a few tens of millions of years at polar latitudes higher than 70 • N and S, and a few hundreds of million years at lower polar latitudes. The ages determined are consistent with the youth of the surface (< 1 Gyr) and the repartition of dissolution-related landforms on Titan.

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Titan from Cassini-Huygens

Cited by 62 publications

References 8 publications

Report of the IAU Working Group on Cartographic Coordinates and Rotational Elements: 2009

Report of the IAU Working Group on Cartographic Coordinates and Rotational Elements: 2009

Saturn’s icy satellites investigated by Cassini-VIMS. IV. Daytime temperature maps

Dissolution on Titan and on Earth: Toward the age of Titan's karstic landscapes

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