Relativistic tests with lunar laser ranging
Relativistic tests with lunar laser ranging
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DOI：
10.1088/1361-6382/aa8f7a
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发表时间：
2018-01
影响因子：
3.5
通讯作者：
F. Hofmann;Jürgen Müller
中科院分区：
文献类型：
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作者：
F. Hofmann;Jürgen Müller
本文介绍了德国莱布尼茨Universität汉诺威研究所（IfE）最新版本的月球激光测距（LLR）分析模型，并重点介绍了利用LLR数据对爱因斯坦引力理论进行的一些测试。对引力常数可能的时间变化、等效原理、PPN参数β和γ以及大地进动进行了研究。利用太阳和行星的引力效应，以月球为扩展体，对LLR分析模型进行了更新。研究了地月之间的高阶引力相互作用以及固体地球潮汐对月球运动的影响。根据DE430星历，现在模拟月球自转的基础是一个2层的地核/地幔模型。使用更新的分析模型和1970年至2015年1月的LLR数据集来研究爱因斯坦理论的有效性。在估计的精度范围内，没有发现与爱因斯坦理论的偏差。重力常数的相对时间变化估计为G˙/G0=（7.1±7.6）×10−14 yr−1，等效原理检验得到Δ（mg/mi）EM=（−3±5）×10−14，Nordtvedt参数η=（−0.2±1.1）×10−4，ppn参数β和γ确定为β−1=（−4.5±5.6）×10−5和γ−1=（−1.2±1.2）×10−4，大地进动在0.09%以内。在不估计相对论量的情况下，通过从LLR解中引入约束，得到了所选相对论参数的结果。在估算G˙/G0、β和γ时，对站坐标进行了约束；在估算G˙/G0和大地进动时，对地核旋转矢量的初始值进行了约束。月球初始速度的受限z分量用于大地进动的估计。
This paper presents the recent version of the lunar laser ranging (LLR) analysis model at the Institut für Erdmessung (IfE), Leibniz Universität Hannover and highlights a few tests of Einstein’s theory of gravitation using LLR data. Investigations related to a possible temporal variation of the gravitational constant, the equivalence principle, the PPN parameters β and γ as well as the geodetic precession were carried out. The LLR analysis model was updated by gravitational effects of the Sun and planets with the Moon as extended body. The higher-order gravitational interaction between Earth and Moon as well as effects of the solid Earth tides on the lunar motion were refined. The basis for the modeled lunar rotation is now a 2-layer core/mantle model according to the DE430 ephemeris. The validity of Einstein’s theory was studied using this updated analysis model and an LLR data set from 1970 to January 2015. Within the estimated accuracies, no deviations from Einstein’s theory are detected. A relative temporal variation of the gravitational constant is estimated as G˙/G0=(7.1±7.6)×10−14 yr−1, the test of the equivalence principle gives Δ(mg/mi)EM=(−3±5)×10−14 and the Nordtvedt parameter η=(−0.2±1.1)×10−4, the PPN-parameters β and γ are determined as β−1=(−4.5±5.6)×10−5 and γ−1=(−1.2±1.2)×10−4 and the geodetic precession is confirmed within 0.09%. The results for selected relativistic parameters are obtained by introducing constraints from an LLR solution without estimating relativistic quantities. The station coordinates are constrained for the estimation of G˙/G0, β and γ, the initial value of the core rotation vector is constrained to a reasonable model value for the estimation of G˙/G0 and geodetic precession. A constrained z-component of the initial lunar velocity is used for the estimation of the geodetic precession.