The heating of the solar chromosphere and corona to the observed high temperatures, imply the presence of ongoing heating that balances the strong radiative and thermal conduction losses expected in the solar atmosphere. It has been theorized for decades that the required heating mechanisms of the chromospheric and coronal parts of the active regions, quiet-Sun, and coronal holes are associated with the solar magnetic fields. However, the exact physical process that transport and dissipate the magnetic energy which ultimately leads to the solar plasma heating are not yet fully understood. The current understanding of coronal heating relies on two main mechanism: reconnection and MHD waves that may have various degrees of importance in different coronal regions. In this review we focus on recent advances in our understanding of MHD wave heating mechanisms. First, we focus on giving an overview of observational results, where we show that different wave modes have been discovered in the corona in the last decade, many of which are associated with a significant energy flux, either generated in situ or pumped from the lower solar atmosphere. Afterwards, we summarise the recent findings of numerical modelling of waves, motivated by the observational results. Despite the advances, only 3D MHD models with Alfv\'en wave heating in an unstructured corona can explain the observed coronal temperatures compatible with the quiet Sun, while 3D MHD wave heating models including cross-field density structuring are not yet able to account for the heating of coronal loops in active regions to their observed temperature.

中文翻译：

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MHD 波的日冕加热

太阳色球层和日冕加热到观察到的高温，意味着持续加热的存在平衡了太阳大气中预期的强辐射和热传导损失。几十年来，人们一直认为活动区、静太阳和日冕洞的色球层和日冕部分所需的加热机制与太阳磁场有关。然而，传输和耗散最终导致太阳能等离子体加热的磁能的确切物理过程尚不完全清楚。目前对日冕加热的理解依赖于两种主要机制：重联和 MHD 波，它们在不同的日冕区域可能具有不同程度的重要性。在这篇综述中，我们重点介绍了我们对 MHD 波加热机制的理解的最新进展。首先，我们重点概述观测结果，我们表明在过去十年中在日冕中发现了不同的波模式，其中许多与显着的能量通量有关，这些能量通量要么是原位产生的，要么是从低层泵浦的。太阳大气。然后，我们总结了最近在观测结果的推动下对波浪进行数值建模的发现。尽管取得了进展，但只有在非结构化日冕中具有阿尔夫恩波加热的 3D MHD 模型才能解释观察到的与安静太阳兼容的日冕温度，