The Concentric Maclaurin Spheroid method with tides and a rotational enhancement of Saturn's tidal response
The Concentric Maclaurin Spheroid method with tides and a rotational enhancement of Saturn's tidal response
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DOI：
10.1016/j.icarus.2016.09.011
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发表时间：
2016-02
期刊：
影响因子：
3.2
通讯作者：
S. Wahl;W. Hubbard;B. Militzer
中科院分区：
文献类型：
--
作者：
S. Wahl;W. Hubbard;B. Militzer
我们扩展到三维的同心麦克劳林球体方法获得自洽的形状和重力场的旋转液体行星，包括潮汐势从卫星。我们表现出，第一次，气体巨星，其形状是由快速旋转的离心势主导的潮汐响应的行星旋转速率的重要影响。对像木星和土星这样自转速度快的行星的模拟，与非自转天体相比，在计算的潮汐爱数k nm上表现出显着的变化。土星的测试模型拟合到观测到的纬向引力多极谐波，得到k 2= 0.413，与卡西尼天体测量数据最近的观测结果一致（Lainey等人，2016年）。在对土星内部自转速率、卫星参数和土星内部结构细节的合理假设下，计算出的勒夫数是稳健的。该方法是基准对几个已发表的测试案例。
We extend to three dimensions the Concentric Maclaurin Spheroid method for obtaining the self-consistent shape and gravitational field of a rotating liquid planet, to include a tidal potential from a satellite. We exhibit, for the first time, an important effect of the planetary rotation rate on tidal response of gas giants, whose shape is dominated by the centrifugal potential from rapid rotation. Simulations of planets with fast rotation rates like those of Jupiter and Saturn, exhibit significant changes in calculated tidal love numbers k nm when compared with non-rotating bodies. A test model of Saturn fitted to observed zonal gravitational multipole harmonics yields k 2= 0.413, consistent with a recent observational determination from Cassini astrometry data (Lainey et al., 2016.). The calculated love number is robust under reasonable assumptions of interior rotation rate, satellite parameters, and details of Saturn’s interior structure. The method is benchmarked against several published test cases.