Meteor impacts and/or meteor events generate body and surface seismic waves on the surface of a planet. When meteoroids burst in the atmosphere, they generate shock waves that subsequently convert into acoustic waves in the atmosphere and seismic waves in the ground. This effect can be modeled as the amplitude of Rayleigh and other Spheroidal modes excitation, due to atmospheric/ground coupling effects.First, an inversion of the seismic source of Chelyabinsk superbolide is performed. We develop an approach in order to model a line source in the atmosphere, corresponding to the consecutive generation of shock waves by the interaction with the atmosphere. The model is based on the known trajectory. We calculate the synthetic seismograms of Rayleigh waves associated with the event by the summation of normal modes of a model of the solid part and the atmosphere of the planet. Through an inversion technique based on singular value decomposition, we perform a full Rayleigh wave inversion and we provide solutions for the moment magnitude.SEIS will likely detect seismic waves generated by impacts and the later might be further located by remote sensing differential processing. In the case of Mars, we use the same method to obtain waveforms associated with impacts on the planetary surface or in low altitudes in the Martian atmosphere. We show that the contribution of the fundamental spheroidal solid mode is dominating the waveforms, compared to that of the first two overtones. We perform an amplitude comparison and we show that small impactors (diameter of 0.5 to 2 m), can be detected by the SEIS VBB seismometer of InSight mission, even in short epicentral distances, in the higher frequencies of the Rayleigh waves. We perform an analysis based on impact rate estimations and we calculate the number of detectable events of 1 meter diameter meteor impacts to be 6.7 to 13.4 per 1 Martian year for a Q=500$Q=500$.

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地球上流星瑞利波的反演和火星上空气耦合瑞利波的建模

流星撞击和/或流星事件在行星表面产生体和地表地震波。当流星体在大气中爆炸时，它们会产生冲击波，随后在大气中转化为声波，在地面上转化为地震波。由于大气/地面耦合效应，这种效应可以模拟为瑞利和其他球体模式激发的振幅。首先，对车里雅宾斯克超流星体的震源进行反演。我们开发了一种方法来模拟大气中的线源，对应于与大气相互作用连续产生的冲击波。该模型基于已知轨迹。我们通过固体部分和行星大气模型的正常模式的总和来计算与事件相关的瑞利波的合成地震图。通过基于奇异值分解的反演技术，我们进行了完整的瑞利波反演，并为矩震级提供了解决方案。SEIS可能会检测到撞击产生的地震波，后者可能会通过遥感差分处理进一步定位。在火星的情况下，我们使用相同的方法来获得与行星表面或火星大气中低空撞击相关的波形。我们表明，与前两个泛音相比，基本球形固体模式的贡献主导了波形。我们进行了振幅比较，结果表明，即使在较短的震中距离和较高频率的瑞利波中，InSight 任务的 SEIS VBB 地震仪也可以检测到小的撞击物（直径为 0.5 到 2 m）。我们根据撞击率估计进行分析，我们计算出 1 米直径流星撞击的可探测事件数量为每 1 个火星年 6.7 到 13.4 次，Q=500$Q=500$。