Bubble streams in Titan’s seas as a product of liquid N2 + CH4 + C2H6 cryogenic mixture
Bubble streams in Titan’s seas as a product of liquid N2 + CH4 + C2H6 cryogenic mixture
复制标题
泰坦海洋中的气泡流是液态 N2 + CH4 + C2H6 低温混合物的产物
作者：
D. Cordier;F. García;D. Justo;G. Liger
土卫六是土星最大的卫星，是已知的唯一一个在其表面支持稳定液体的外星天体，其形式是点缀在极地地区的海洋和湖泊。许多迹象表明，这种液体应该是由氮气、甲烷和乙烷的混合物组成的。卡西尼号的无线电探测和测距（RADAR）仪器最近对泰坦的大型海洋进行了观测，称为Ligeia Mare，显示出无法解释的短暂明亮特征，可能是由于气泡上升。在这里，我们报告说，我们的数值模型，当结合文献中发现的实验数据，表明丽姬亚海的床是一个有利的地方氮出溶。这个过程可以产生厘米大小的雷达可探测的气泡。液态甲烷湖点缀着土卫六的极地。数值模型表明，通过氮出溶附近的丽姬亚马雷湖床浮力气泡的创建可以解释卡西尼号在湖面上观察到的瞬态增亮。
Titan, Saturn’s largest moon, is the only extraterrestrial body known to support stable liquid on its surface, in the form of seas and lakes that dot the polar regions. Many indications suggest that the liquid should be composed of a mixture of nitrogen, methane and ethane. Recent observations by Cassini’s Radio Detection and Ranging (RADAR) instrument of Titan’s large sea, called Ligeia Mare, have shown unexplained and ephemeral bright features, possibly due to rising bubbles. Here we report that our numerical model, when combined with experimental data found in the literature, shows that Ligeia Mare’s bed is a favourable place for nitrogen exsolution. This process could produce centimetre-sized and RADAR-detectable bubbles. Liquid methane lakes dot Titan’s polar regions. Numerical models reveal that the creation of buoyant bubbles through nitrogen exsolution near the bed of the Ligeia Mare lake can explain transient brightenings observed by Cassini on the lake’s surface.
泰坦烃海潮汐和海洋角动量的数值模拟
影响因子：
3.2
作者：
Tokano;Lorenz;Van Hoolst
通讯作者：
Van Hoolst