Structure and Dynamics of the Quiet Chromosphere

安静色球层的结构和动力学

• 批准号: 0207641
• 负责人: Wolfgang Kalkofen
• 金额: $ 2.93万
• 依托单位: Smithsonian Institution Astrophysical Observatory
• 依托单位国家: 美国
• 项目类别: Standard Grant
• 财政年份: 2002
• 资助国家: 美国
• 起止时间: 2002-09-01 至 2004-08-31
• 项目状态: 已结题
• 来源: https://www.nsf.gov/awardsearch/showAward?AWD_ID=0207641&HistoricalAwards=false
• 关键词: Structure; Dynamics; Quiet; Chromosphere

This investigation will address the question: Is the quiet solar chromosphere at the top always hot (7000 K), with small temperature variations (5%), or mainly cold (2000 K), with large temperature excursions (up to 25,000 K)? Two kinds of current empirical models, one a set of time-independent models of the steady emission, the other, a time-dependent simulation of the dynamics of the non-magnetic chromosphere, come to fundamentally different conclusions. To gain a resolution of this problem a two-pronged approach will be employed. On the one hand, space observations are to be analyzed to determine the temperature and the amplitude of oscillations in the actual solar chromosphere, and on the other, numerical and analytic tools will be developed for a theoretical assessment of chromospheric heating by magnetohydrodynamic waves.

这项研究将解决的问题：是安静的太阳色球层顶部总是热（7000 K），与小的温度变化（5%），或主要是冷（2000 K），与大的温度漂移（高达25,000 K）？ 目前的两种经验模型，一组与时间无关的稳定发射模型，另一组与时间相关的非磁性色球层动力学模拟，得出了根本不同的结论。 为解决这一问题，将采取双管齐下的办法。 一方面，将对空间观测进行分析，以确定实际太阳色球层中的温度和振荡幅度，另一方面，将开发数值和分析工具，对磁流体动力波引起的色球层加热进行理论评估。