Theoretical Models of the Solar Chromosphere, Transition Region and Wind

太阳色球层、过渡区和风的理论模型

• 批准号: 0087184
• 负责人: Zdzislaw Musielak
• 金额: $ 28.86万
• 依托单位: University of Texas at Arlington
• 依托单位国家: 美国
• 项目类别: Continuing Grant
• 财政年份: 2001
• 资助国家: 美国
• 起止时间: 2001-04-01 至 2005-08-31
• 项目状态: 已结题
• 来源: https://www.nsf.gov/awardsearch/showAward?AWD_ID=0087184&HistoricalAwards=false
• 关键词: Theoretical; Models; Solar; Chromosphere; Transition

The investigators will determine which heating mechanisms dominate in different regions of the solar atmosphere. The main effort is to construct novel theoretical models that will describe the entire solar atmosphere. Observations show that the solar atmosphere can be divided into three main regions: chromosphere, transition region and corona. In each of these regions the temperature increases with height and reaches its maximum in the corona, where both X-ray emission and the solar wind originate. One of the most important, and still unsolved, problems in solar physics is to identify the basic physical processes that are responsible for this heating. There are at least two general classes of models of this heating. In the first class, the solar atmosphere is heated by hydrodynamic (mainly acoustic) or magnetohydrodynamic (MHD) waves, and it is assumed that these waves are generated by turbulent motions in the solar convection zone. In the second class, dissipation of currents generated by photospheric motions of solar magnetic fields is the primary source of energy for the heating. Despite the vast amount of solar data collected during numerous ground observations and space missions, and significant theoretical efforts, it is still unclear how different regions of the solar atmosphere actually are heated. The investigators will take a novel approach to this problem by constructing theoretical models that describe the entire solar atmosphere. By comparing these models with observations, they will determine which heating mechanisms dominate in different regions of the solar atmosphere. Their work will be important in ongoing efforts to understand the principal energy sources for the solar atmosphere and the basic physical processes responsible for creating the heliosphere.

研究人员将确定哪些加热机制在太阳大气的不同区域占主导地位。主要的努力是建立新的理论模型，将描述整个太阳大气。观测表明，太阳大气可分为三个主要区域：色球层、过渡区和日冕。在这些区域中的每一个，温度都随着高度的增加而增加，并在日冕中达到最高值，X射线发射和太阳风都起源于日冕。太阳物理学中最重要的问题之一，也是尚未解决的问题之一，就是确定导致这种加热的基本物理过程。这种加热至少有两种一般类型的模型。在第一类中，太阳大气被流体动力学（主要是声学）或磁流体动力学（MHD）波加热，并假设这些波是由太阳对流区的湍流运动产生的。在第二类中，太阳磁场光球运动产生的电流耗散是加热的主要能量来源。尽管在许多地面观测和太空任务中收集了大量的太阳数据，以及重要的理论工作，但仍然不清楚太阳大气层的不同区域实际上是如何加热的。研究人员将通过构建描述整个太阳大气的理论模型来解决这个问题。通过将这些模型与观测结果进行比较，他们将确定哪些加热机制在太阳大气的不同区域占主导地位。他们的工作将对正在进行的了解太阳大气层的主要能源和形成日光层的基本物理过程的努力具有重要意义。