Chromospheric and coronal heating mechanisms with emphasis on microflare heating

色球层和日冕加热机制，重点是微耀斑加热

• 批准号: 5405479
• 负责人: Professor Dr. Peter Ulmschneider
• 金额: --
• 依托单位国家: 德国
• 项目类别: Research Grants
• 财政年份: 2003
• 资助国家: 德国
• 起止时间: 2002-12-31 至 2003-12-31
• 项目状态: 已结题
• 来源: https://gepris.dfg.de/gepris/projekt/5405479?language=en
• 关键词: Chromospheric; coronal; heating; mechanisms; emphasis

After reviewing some time ago the important heating mechanisms of chromospheric and coronal heating a new summary of recent developments is urgently needed. Since acoustic and magnetohydrodynamic wave heating are now much better understood it is particularly important to place an emphasis on non-wave heating mechanisms. Recent theoretical research as well as observations of coronal heating suggests that microflares are such a mechanism which operates in the chromosphere-corona transition layer at the base of the corona. It is generated by small scale reconnection events brought about by the foot point motions of coronal magnetic flux tubes in a crowded tube forest-like situation. This mechanism most likely is a candidate fot the next most important heating mechanism after wave heating. With a thorough search of the literature we want to review the whole spectrum of heating mechanisms. We also want to generate a phenomenological model fot the microflare event which can be taken as basis for an intended time-dependent multidimensional magnetohydrodynamic simulation. For this collaboration the Indian National Academy has already awarded some support.

在回顾了前段时间色球和日冕加热的重要加热机制之后，迫切需要对最近的发展进行新的总结。由于现在对声波加热和磁流体动力波加热有了更好的理解，因此强调非波加热机制尤为重要。最近的理论研究以及日冕加热的观察表明，微耀斑是一种在日冕底部的色球层-日冕过渡层中运行的机制。它是由拥挤的管森林状情况下日冕磁通量管的足点运动引起的小规模重联事件产生的。这种机制很可能是继波加热之后下一个最重要的加热机制的候选者。通过彻底检索文献，我们希望回顾整个加热机制。我们还希望为微耀斑事件生成一个唯象模型，该模型可以作为预期的时间相关多维磁流体动力学模拟的基础。对于此次合作，印度国家科学院已经提供了一些支持。