T P a D Xanadu Belet Xanadu Adiri

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TITAN Ligeia Mare Kraken Mare L eil ah FlucTus M enrva E liv aga r Fl umina Ksa Sinlap Xanadu FENSAL B e l e t Adiri Xanadu 1° 1° 0° 0° L-1° L-1° 1° 0° 181° 359° 179° 180° Senkyo Guabonito AZTLAN Huygens Ontario Lacus Arrakis Planitia M E Z Z OR A M I A FA SUR CE 779 57 -180°C SUN 3 T T MERCURY E EM R JUPITER EARTH PERATU DENSITY 5.51 g/cm GRAVITY Titan ESSURE 150 EARTH 2 PR 9.81 m/s DENSITY 1.88 g/cm GRAVITY 108 1.35 m/s2 P 1467 mb 3 URANUS FA UR CE S VENUS . S O Titan is the largest moon of Saturn, the ringed planet. This is the only L A 2 R LENGTH OF EQuatOR 40 075 km moon with a thick atmosphere. The material on Titan’s surface consists of 83 305 418 km 228 D A IS water-ice; that is, its rocks are also made of ice. Titan’ interior is not hot TA SAMPLE A A N R E CE RETURN now, so there are no active volcanoes on it. There are still a lot of changes : 14 LENGTH OF EQuatOR 16 177 km 26 C N happening to its surface, which is mainly caused by the methane cycle. There M 2 SOLAR COnstant OMPOSITIO AMETER MARS IL Saturn DI LIO SOLAR COnstant OF THE ATMOSPHERE is no liquid water on Titan because the material of ice-rock is always in a 5148 km N K 1361 W/m 15 W/m M COMPOSITION 2 state frozen to the hardness of rock at the cold surface (-180°C). The role of OF T RE 95% N2 d S HE ATMOSPHE 23:56 15.9d ground water on Earth is performed by ethane and methane on Titan. Methane Y A NEPTUNE 5% CH4 D 78% N 1% O Titan 5 2, 2 2 on the Earth occurs only as a gas, as for example in the flame of a gas stove. 1 R T: 1% Ar, 0.04% CO2 There is also methane rain falling from Titan’s clouds; when it accumulates, it EV NE ICE PEBBLES OL A UTI PL forms rivers, which run into polar lakes and seas. In the region of the equator, ON ARO ND THE U parallel bands of dark dunes line up and bury much of the surface. Titan’s landscapes are perhaps the most similar to the Earth within the solar system, but still it is a planet that operates very differently from ours. Space probe MAP OF TITAN. Lambert Azimuthal Equal Area Projection. 1 : 16 000 000 (1 cm = 160 km) Editor: Henrik Hargitai. Graphic artist: Panka Pásztohy. EARTH Titan Huygens landed on its surface in 2005. It is the farthest world from the sun Technical review: Jim Zimbelman. Supporters: Europlanet 2012 Outreach Funding Scheme, Paris Observatory, International Cartographic Association Commission on Planetary Cartography. Published by Eötvös Loránd University, Budapest. ISBN 978-963-284-438-1, [PDF] ISBN 978-963-284-437-4. on which photos of its surface have ever been taken. Illustration © Panka Pásztohy 2014. Text © Henrik Hargitai 2014. http://childrensmaps.wordpress.com.

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Cassini RADAR Images at Hotei Arcus and Western Xanadu, Titan: Evidence for Geologically Recent Cryovolcanic Activity S
GEOPHYSICAL RESEARCH LETTERS, VOL. 36, L04203, doi:10.1029/2008GL036415, 2009 Click Here for Full Article Cassini RADAR images at Hotei Arcus and western Xanadu, Titan: Evidence for geologically recent cryovolcanic activity S. D. Wall,1 R. M. Lopes,1 E. R. Stofan,2 C. A. Wood,3 J. L. Radebaugh,4 S. M. Ho¨rst,5 B. W. Stiles,1 R. M. Nelson,1 L. W. Kamp,1 M. A. Janssen,1 R. D. Lorenz,6 J. I. Lunine,5 T. G. Farr,1 G. Mitri,1 P. Paillou,7 F. Paganelli,2 and K. L. Mitchell1 Received 21 October 2008; revised 5 January 2009; accepted 8 January 2009; published 24 February 2009. [1] Images obtained by the Cassini Titan Radar Mapper retention age comparable with Earth or Venus (500 Myr) (RADAR) reveal lobate, flowlike features in the Hotei [Lorenz et al., 2007]). Arcus region that embay and cover surrounding terrains and [4] Most putative cryovolcanic features are located at mid channels. We conclude that they are cryovolcanic lava flows to high northern latitudes [Elachi et al., 2005; Lopes et al., younger than surrounding terrain, although we cannot reject 2007]. They are characterized by lobate boundaries and the sedimentary alternative. Their appearance is grossly relatively uniform radar properties, with flow features similar to another region in western Xanadu and unlike most brighter than their surroundings. Cryovolcanic flows are of the other volcanic regions on Titan. Both regions quite limited in area compared to the more extensive dune correspond to those identified by Cassini’s Visual and fields [Radebaugh et al., 2008] or lakes [Hayes et al., Infrared Mapping Spectrometer (VIMS) as having variable 2008].
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The Lakes and Seas of Titan • Explore Related Articles • Search Keywords Alexander G
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