On the Impact Origin of Phobos and Deimos. I. Thermodynamic and Physical Aspects
On the Impact Origin of Phobos and Deimos. I. Thermodynamic and Physical Aspects
复制标题
DOI：
10.3847/1538-4357/aa81c4
复制
发表时间：
2017-08-20
影响因子：
4.9
通讯作者：
Rosenblatt, Pascal
中科院分区：
文献类型：
--
作者：
Hyodo, Ryuki;Genda, Hidenori;Rosenblatt, Pascal
火卫一和土卫二是火星上的两个小卫星。最近的研究表明，它们可以在撞击产生的圆盘内共生。然而，人们对圆盘的详细结构和初始热力学性质知之甚少。在这篇文章中，我们对火星上形成月球的巨型撞击进行了高分辨率的SPH模拟，这种撞击也可以形成北冰洋盆地。这个巨大的撞击加热了圆盘材料(大约类似于2000 K的温度)，熵增加了大约1500 JK(-1)kg(-1)。因此，磁盘材料应该大部分是熔融的，尽管有一小部分磁盘材料(
Phobos and Deimos are the two small moons of Mars. Recent works have shown that they can accrete within an impact-generated disk. However, the detailed structure and initial thermodynamic properties of the disk are poorly understood. In this paper, we perform high-resolution SPH simulations of the Martian moon-forming giant impact that can also form the Borealis basin. This giant impact heats up the disk material (around similar to 2000 K in temperature) with an entropy increase of similar to 1500 JK(-1) kg(-1). Thus, the disk material should be mostly molten, though a tiny fraction of disk material (