The Water–Ammonia Phase Diagram up to 300 MPa: Application to Icy Satellites
The Water–Ammonia Phase Diagram up to 300 MPa: Application to Icy Satellites
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DOI：
10.1006/icar.2002.6932
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发表时间：
2002-10
期刊：
影响因子：
3.2
通讯作者：
J. Leliwa-kopystyński;M. Maruyama;T. Nakajima
中科院分区：
文献类型：
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作者：
J. Leliwa-kopystyński;M. Maruyama;T. Nakajima
我们在氨-水（NH3）x(H2O)（1−x）体系中对水冰I和水冰III的结晶进行了高压实验，并将结果应用于太阳系冰体内部。在全液体溶液和有水形成冰的液体溶液之间的相平衡线（液相线）被确定为氨浓度的质量X等于0.034,0.0472,0.111,0.176和0.229。观察到冰I和冰III晶体的生长-融化。将结果应用于可能携带氨的冰冻卫星上，结果表明氨的掺入降低了液面深度。卫星内液体温度的变化取决于三个参数：氨浓度X；温度梯度，α；密度和重力的乘积，ρg。
We performed high-pressure experiments on the crystallization of water ice I and III in the ammonia–water (NH3)x(H2O)(1−x) system, and apply the results to the interiors of icy bodies in the Solar System. Phase equilibrium lines between an entirely liquid solution and a liquid solution in which water ice forms (liquidus lines) were determined for ammonia concentration by mass X equal to 0.034, 0.0472, 0.111, 0.176, and 0.229. Growth–melting of ice I as well as ice III crystals were observed. Application of the results to icy satellites that are potential bearers of ammonia shows that ammonia admixture decreases the depth of the liquidus surface. A shift of the liquidus temperature within a satellite depends on three parameters: the ammonia concentration, X; the temperature gradient, α; and the product of density and gravity, ρg.