木星地震学的正反演模拟
Forward and Inverse Modeling for Jovian Seismology
摘要：
预计木星将在声学模式的频谱中脉动，最近对光谱时间序列的重新分析已经确定了频率\citep{gaulme2011}间隔的规则模式。这一令人兴奋的结果可以提供对木星总属性的限制，并保证对木星地震结构进行更深入的理论研究。使用当前的仪器，例如用于\citet{gaulme2011}分析的SYMPA仪器\citep{schmider2007}，我们假设至少可以观察到一组扩展到角度$\ell=25$的全局频率。为了确定哪些模式将最好地约束模型的木星的内部，从而有助于激励下一代的观测，我们探讨了导出的参数的敏感性，这种模式集。计算了木星内部的三种不同模型，并从这些模型中得到了$\ell\leq 25$的理论脉动谱。我们计算灵敏度内核和执行线性反演，以推断在木星内部的配置文件中的预期不连续的细节。我们发现，在两个应用模型中看到的内/外包络边界中的几个百分点的声速跳跃的幅度应该合理地推断出这些特定的模式。在模型预测的大密度不连续性的核心边界附近，这些特征的位置可以被准确地测量，而它们的振幅具有更大的不确定性。这些结果表明，这种模式集足以推断木星内部预期不连续性的径向位置和强度，并对核心大小和质量施加强有力的约束。我们鼓励新的观测来探测这些木星振荡。
英文摘要：
Jupiter is expected to pulsate in a spectrum of acoustic modes and recent re-analysis of a spectroscopic time series has identified a regular pattern in the spacing of the frequencies \citep{gaulme2011}. This exciting result can provide constraints on gross Jovian properties and warrants a more in-depth theoretical study of the seismic structure of Jupiter. With current instrumentation, such as the SYMPA instrument \citep{schmider2007} used for the \citet{gaulme2011} analysis, we assume that, at minimum, a set of global frequencies extending up to angular degree $\ell=25$ could be observed. In order to identify which modes would best constrain models of Jupiter's interior and thus help motivate the next generation of observations, we explore the sensitivity of derived parameters to this mode set. Three different models of the Jovian interior are computed and the theoretical pulsation spectrum from these models for $\ell\leq 25$ is obtained. We compute sensitivity kernels and perform linear inversions to infer details of the expected discontinuities in the profiles in the Jovian interior. We find that the amplitude of the sound-speed jump of a few percent in the inner/outer envelope boundary seen in two of the applied models should be reasonably inferred with these particular modes. Near the core boundary where models predict large density discontinuities, the location of such features can be accurately measured, while their amplitudes have more uncertainty. These results suggest that this mode set would be sufficient to infer the radial location and strength of expected discontinuities in Jupiter's interior, and place strong constraints on the core size and mass. We encourage new observations to detect these Jovian oscillations.
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