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

利用数值模拟对磁化太阳大气中的内部重力波进行综合研究

基本信息

批准号：
317162715
负责人：
Professor Dr. Markus Roth
金额：
--
依托单位：
Thüringer Landessternwarte Tautenburg (TLS) - Karl-Schwarzschild-Observatorium
依托单位国家：
德国
项目类别：
Research Grants
财政年份：
2016
资助国家：
德国
起止时间：
2015-12-31 至 2019-12-31
项目状态：
已结题

来源：
https://gepris.dfg.de/gepris/projekt/317162715?language=en
关键词：
comprehensive study internal gravity waves

项目摘要

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.

太阳复杂的磁大气层支持不同类型的波。这些磁大气波部分地负责太阳外层的质量和能量平衡。但是，磁流体动力学过程的产生，传播和这些波的耗散知之甚少。对所有不同波动现象的清晰认识对于解决围绕太阳的各种谜团至关重要，包括上层加热问题。这方面的研究重新引起了人们对内部重力波的兴趣，人们认为内部重力波能够将足够的能量转移到上层，以平衡通过辐射损失的能量。然而，对真实的太阳的观测表明，这些波在强磁场区域被抑制。这就提出了关于它们的全球影响力的问题，因为太阳大气层被各种可能尺度的磁场所渗透。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经过的磁化环境的性质。我们认为，这种耦合可以提供一个途径，内部重力波可以间接地有助于太阳大气的整体能量收支。借助最先进的数值模拟，我们将对真实太阳模型中内部重力波的产生和传播进行全面研究（项目的第一和第二部分）。研究具有空间和时间变化磁场的大气中这些波的特性将使我们更接近太阳上发生的实际过程。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太阳真实的观测数据，并从观测者的角度研究它们的性质（第三部分）。这将导致对当前和未来观测的更好解释，并将进一步推进我们对太阳大气中波作用的认识。在更广泛的背景下，拟议工作的预期意义是将我们对太阳大气中所有不同波现象的理解中缺失的环节与它们在直接或间接维持能量平衡方面的单独作用联系起来，并揭示磁化太阳大气的性质。