Lorenz R D, Wall S, Radebaugh J, Boubin G, Reffet E, Janssen M, Stofan E, Lopes R, Kirk R, Elachi C, Lunine J, Mitchell K, Paganelli F, Soderblom L, Wood C, Wye L, Zebker H, Anderson Y, Ostro S, Allison M, Boehmer R, Callahan P, Encrenaz P, Ori G G, Francescetti G, Gim Y, Hamilton G, Hensley S, Johnson W, Kelleher K, Muhleman D, Picardi G, Posa F, Roth L, Seu R, Shaffer S, Stiles B, Vetrella S, Flamini E, West R
Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ 85721, USA.
Science. 2006 May 5;312(5774):724-7. doi: 10.1126/science.1123257.
The most recent Cassini RADAR images of Titan show widespread regions (up to 1500 kilometers by 200 kilometers) of near-parallel radar-dark linear features that appear to be seas of longitudinal dunes similar to those seen in the Namib desert on Earth. The Ku-band (2.17-centimeter wavelength) images show approximately 100-meter ridges consistent with duneforms and reveal flow interactions with underlying hills. The distribution and orientation of the dunes support a model of fluctuating surface winds of approximately 0.5 meter per second resulting from the combination of an eastward flow with a variable tidal wind. The existence of dunes also requires geological processes that create sand-sized (100- to 300-micrometer) particulates and a lack of persistent equatorial surface liquids to act as sand traps.
卡西尼号最近拍摄的土卫六雷达图像显示，存在广泛区域（长达1500公里，宽200公里）的近乎平行的雷达暗线性特征，这些特征似乎是纵向沙丘形成的海洋，类似于地球上纳米布沙漠中所见的沙丘。Ku波段（波长2.17厘米）图像显示出约100米的脊，与沙丘形态一致，并揭示了与下层山丘的流动相互作用。沙丘的分布和方向支持这样一种模型：由向东流动与变化的潮汐风相结合产生的约每秒0.5米的波动表面风。沙丘的存在还需要地质过程来产生沙粒大小（100至300微米）的颗粒，并且缺乏持续的赤道表面液体来充当沙阱。
