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月球的潮旋转形状和极地漫游的证据
Ian Garrick-Bethell1, Viranga Perera2, Francis Nimmo3
11] Department of Earth and Planetary Sciences, University of California, Santa Cruz, 1156 High Street, Santa Cruz, California 95064, USA [2] School of Space Research, Kyung Hee University, 1 Seocheon-dong, Giheung-gu, Yongin-si, Gyeonggi-do 446-701, Korea.
Nature
|August 1, 2014
概括
月球的形状是由早期的潮加热和后来结的潮凸起解释的,而不仅仅是冲击. 这一过程也导致月球的极轴随着时间的推移而显著转移.
科学领域:
- 月球地质学和地质物理学.
- 星球科学 星球科学
- 地力学是什么?地力学是什么?
背景情况:
- 月球大尺度地形的起源对于理解它的地质,轨道演变和方向至关重要.
- 以前的假设包括晚期积累,冲击,潮效应和对流,但大盆地使分析复杂化.
研究的目的:
- 为了估计月球的大规模地形和重力,在主要盆地以外的球体波.
- 测试有关月球形状及其地质历史的假设.
主要方法:
- 分析月球地形和重力球体波,不包括大型撞击盆地.
- 模拟潮加热和潮旋转膨胀效应.
主要成果:
- 2度的地形主要与地形成期间的早期潮加热相一致.
- 2度地形的次要组成部分与以后的结的潮旋转凸起相匹配,距离地球半径约32度.
- 内部密度对比将月球的极轴重新定位36±4°.
结论:
- 月球的形状最好解释为早期的潮加热和后来结的潮凸起的组合.
- 这些过程将月球地质联系起来,并解决有关月球形状,重力和极地漫游历史的问题.
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