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首页> 外文期刊>The Astrophysical journal >FORWARD MODELING OF ACOUSTIC WAVE PROPAGATION IN THE QUIET SOLAR SUBPHOTOSPHERE
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FORWARD MODELING OF ACOUSTIC WAVE PROPAGATION IN THE QUIET SOLAR SUBPHOTOSPHERE

机译：安静的太阳水下球面声波传播的正演模拟

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摘要

The results of numerical simulations of acoustic wave propagation and dispersion in the nonmagnetic solar sub-photosphere are presented. Initial equilibrium density and pressure stratifications are taken from a standard solar model but modified to suppress convective instabilities in fully compressible two-dimensional ideal hydrodynam-ical modeling. Acoustic waves are generated by sources located below the height corresponding to the visible solar surface. The dynamic response of the solar interior to two acoustic source types, namely a harmonic source and one representing downward-propagating photospheric plumes, is studied. A large number of randomly distributed localized cooling sources with random amplitudes is also introduced. The methods used to analyze the simulation data are similar to ones used in observational studies in local helioseismology. Time-distance diagrams of the pressure and vertical velocity perturbations at the level corresponding to the solar surface show the appearance of wave packets propagating with different speeds, which are reflected at different depths beneath the subphotosphere. The (ω, k_h) power spectra, derived from the vertical velocity data, show the existence of g-,f-, and p-modes; p-mode ridges are identifiable up to high radial orders of n ≈ 11; g-modes appear in the simulations, unlike in the real Sun, where they cannot propagate in the convectively unstable solar subphoto sphere. Cross-correlation analysis of vertical velocity perturbations shows a good correspondence with the observed time-distance helioseismic data for quiet Sun. Thus, the ability of the implemented approach of forward modeling to investigate propagation of acoustic, internal, and surface gravity waves in a realistic solar interior model is shown.
机译：给出了声波在非磁性太阳亚光圈中传播和扩散的数值模拟结果。初始平衡密度和压力分层取自标准太阳模型，但经过修改以抑制在完全可压缩的二维理想水动力模型中的对流不稳定性。声波由位于与可见太阳表面相对应的高度以下的源产生。研究了太阳能内部对两种声源类型的动态响应，即谐波源和一种代表向下传播的光球羽流。还引入了大量具有随机振幅的随机分布的局部冷却源。用于分析模拟数据的方法与用于局部日震学的观测研究相似。压力和垂直速度扰动在与太阳表面相对应的水平处的时距图显示了以不同速度传播的波包的出现，这些波包在亚光圈下的不同深度处反射。从垂直速度数据得出的（ω，k_h）功率谱表明存在g模式，f模式和p模式。在最高n≈11的高径向阶中，可以识别出p型脊。 g模式出现在模拟中，这与真实的太阳不同，在真实的太阳中，它们无法在对流不稳定的太阳副光球中传播。垂直速度摄动的互相关分析表明，它与观测到的安静太阳的时距流变数据有很好的对应关系。因此，显示了已实现的前向建模方法研究现实的太阳能内部模型中的声波，内部和表面重力波传播的能力。

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