A comprehensive study of internal gravity waves in magnetized solar atmosphere using numerical simulations

太阳复杂的磁层支持不同类型的波。这些磁层大气波对太阳S外层包层的质量和能量平衡负有部分责任。但控制这些波的产生、传播和消散的磁流体动力学过程却知之甚少。清楚地了解所有不同的波动现象对于解开围绕太阳的各种谜团至关重要，包括上层的加热问题。在这个方向上的研究重新唤起了人们对内部重力波的兴趣，这种内部重力波被认为能够将足够的能量转移到上层，以平衡辐射损失的能量。然而，对真实太阳的观测表明，这些波在强磁场区域被抑制。这引发了关于它们在全球范围内影响的问题，因为太阳大气被各种可能的磁场渗透。最近使用射线理论的工作表明，内部重力波可以转换为其他磁大气波，这取决于它们传播所通过的磁化环境的性质。我们认为，这种耦合可以提供一种途径，通过这种途径，内重力波可以间接地对太阳大气的整体能量收支做出贡献。借助最先进的数值模拟，我们将全面研究现实太阳模型(项目的第一部分和第二部分)中内重力波的产生和传播。研究具有时空变化磁场的大气中这些波的特性将使我们更接近发生在太阳上的实际过程。作为向前迈出的重要一步，我们将使用我们的模拟模型来合成模拟真实太阳观测的数据，并从观察者S的角度研究它们的性质(第三部分)。这将更好地解释目前和未来的观测结果，并将进一步促进我们对波在太阳大气中的作用的了解。拟议的工作在更广泛的背景下的预期意义是，将我们对太阳大气中所有不同波动现象及其在直接或间接维持能量平衡方面的个别作用以及它们揭示磁化太阳大气性质的潜力的理解中缺失的一环联系起来。

The complex magnetic atmosphere of the Sun supports different types of waves. These magneto-atmospheric waves are partially responsible for the mass and energy balance of the Sun´s outer envelope. But the magneto-hydrodynamic processes governing the generation, propagation, and dissipation of these waves are poorly understood. A clear knowledge of all the different wave phenomena is vital for solving the various mysteries surrounding the Sun, including the problem of heating of the upper layers. Research in this direction had revived interest in internal gravity waves, which are thought to be capable of transferring sufficient energy to the upper layers to balance the energy lost through radiation. However, observations of the real Sun show that these waves are suppressed in strong magnetic field regions. This raises questions about their global influence as the solar atmosphere is permeated by magnetic fields on every possible scale. Recent work using ray theory show that internal gravity waves can convert to other magneto-atmospheric waves depending on the properties of the magnetized environment through which they propagate. We propose that this coupling can provide a pathway by which internal gravity waves can indirectly contribute to the overall energy budget of the solar atmosphere. With the help of state-of-the-art numerical simulations, we will carry out a comprehensive study of the generation and propagation of internal gravity waves in realistic solar models (first and second part of the project). Investigating the properties of these waves in an atmosphere with spatially and temporally varying magnetic fields will bring us more close to the actual processes that happen on the Sun. As a major step forward, we will use our simulated models to synthesize data that mimic real observations of the Sun and study their properties from an observer´s viewpoint (third part). This will lead to a better interpretation of current and future observations and will further advance our knowledge on the role of waves in solar atmosphere. The expected significance of the proposed work on a broader context is to connect the missing link in our understanding of all the different wave phenomena in the solar atmosphere and their individual role in maintaining the energy balance, either directly or indirectly, and their potential for revealing the nature of magnetized solar atmosphere.