Lunar and Planetary Science XXXVII ( 2006 ) 1293 . pdf
Lunar and Planetary Science XXXVII ( 2006 ) 1293 . pdf
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月球与行星科学三十七（2006）1293。
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发表时间：
2006
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通讯作者：
Grindrod
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作者：
A. Fortes;Grindrod
简介：土卫六的内部结构由一个冰冷的地幔覆盖，上面覆盖着一个深含氨水的海洋。1]。考虑到低温火山泰坦的可能性[2]，这显然是集中在氨水作为低温岩浆。对V氨-水混合物的测量已用于泰坦上的低温火山和流动，以及陆地玄武岩的类似物[3]。Indee候选火山建筑，Ganesa Mac伴生流动沉积物，与太阳系其他地方的沉积物相比，[4]TITA中已知的氨的初始数量，值从18wt%组分[5]到基本上为零[6]。该范式也忽略了木星卫星探索的土卫六核心在分化过程中的挥发性组分(主要是硫酸盐)之间的可能性。在这里，我们考虑卡吉尔的模型对伽利略卫星的影响，即从含有氨的球粒陨石核心中浸出硫酸盐。Titan的一种新的内部结构：一个球粒陨石核心产生高达10wt%(主要是MgSO4)的自由进入，所以早期Sa挥发性组分的液体挥发性成分是水，Am甲烷，我们在溶液中固定NH3：CH4=1可溶的硫酸盐与Am水反应生成可溶的硫酸铵a氢氧化物。现在的质量和密度是从0.82的初始岩石中复制出来的；12.7w的氨丰度导致了从1-18wt%的内部氨丰度的完整消耗模型，其中很大一部分被转化为氮气，从泰坦历史的早期就消失了。由此推测，土卫六的所有原始Am都已与硫酸盐反应生成氨。土卫六的模型内部结构分化由一个被深液态地幔覆盖的1990公里的球粒陨石组成，一个硫酸铵的水溶液，一个饱和的甲烷，遍及佤邦，不溶于水的氢氧化物在底部沉淀了约40公里厚的沉积层。土卫六还有一个炎热的厚大气，月球和行星科学XXXVII(2006)1293 pdf
Introduction: The existing paradig the internal structure of Titan consists of overlain by an icy mantle bearing a deep ocean of aqueous ammonia [e.g., ref. 1]. regarding the possibility of cryovolcanic Titan [2], which is now apparently being b focused upon aqueous ammonia as cryomagma. Measurements of the v ammonia-water mixtures have been used cryovolcanoes and flows on Titan wi terrestrial basaltic analogues [3]. Indee candidate volcanic edifice, Ganesa Mac associated flow deposits, bear comparison deposits elsewhere in the solar system [4] the initial quantity of ammonia within Tita known, values ranging between 18 wt % component [5] to essentially zero [6]. paradigm also overlooks the plausible between the volatile fraction of Titan an soluble components (mostly sulfates) in th core during differentiation, as explored by the Jovian moons [7]. Here, we consider the consequences Kargel’s model for the Galilean moons, i leaching of sulfates from a chondritic core, containing ammonia. A new internal structure for Titan: that a chondritic core yields up 10 wt % (mostly MgSO4) that are free to go into so liquid volatile component of the early sa volatile component consists of water, am methane, and we fix NH3:CH4 = 1 fo Soluble sulfates in solution react with am water to form soluble ammonium sulfate a hydroxides. The present mass and density be reproduced from an initial rock mass 0.82; an ammonia abundance of 12.7 w volatile fraction leads to complete consump Models of the ammonia abundance inside from 1 – 18 wt %, of which a large fractio been converted to N2 and lost from the early in Titan’s history. Thus it is re hypothesise that all of Titan’s primordial am have reacted with sulfates to form ammoniu Titan’s model internal structure differentiation consists of a chondritic co 1990 km overlain by a deep liquid mantle an aqueous solution of ammonium sulfate a methane at saturation throughout the wa insoluble hydroxides have precipitated ou sediment layer ~ 40 km thick at the base o Titan also has a hot thick atmosphere Lunar and Planetary Science XXXVII (2006) 1293.pdf