Mysterious Activities of Our Magnificent Sun

我们壮丽的太阳的神秘活动

• 批准号: 0538278
• 负责人: Zdzislaw Musielak
• 金额: $ 25.02万
• 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: 2005
• 资助国家: 美国
• 起止时间: 2005-12-15 至 2010-03-31
• 项目状态: 已结题
• 来源: https://www.nsf.gov/awardsearch/showAward?AWD_ID=0538278&HistoricalAwards=false
• 关键词: Mysterious; Activities; Our; Magnificent; Sun

With previous NSF support, the PI has constructed theoretical models of the solar chromosphere. He has identified acoustic waves as sources of the heating of non-magnetic regions, and longitudinal and transverse tube waves as sources of the heating of magnetic flux tubes; both acoustic and magnetic waves were generated in the solar convection zone. The PI's main conclusion was that the waves alone could not supply enough energy to explain all activity observed in the uppermost chromospheric layers, the solar transition region, and in the solar corona. He also constructed theoretical models of the solar wind that were based on momentum deposition by magnetic waves, and he found that a force exerted by these waves on the background medium contributed significantly to the acceleration of the solar wind.The identification of heating mechanisms operating in the solar atmosphere and the explanation of solar activity resulting from this heating are important and still unsolved problems in solar physics research. The PI proposes to attack these problems by developing a novel approach allowing him to construct models to describe the entire solar atmosphere and account for atmospheric oscillations. The proposed models will be theoretical, self-consistent, and time-dependent, and they will be constructed after comprehensive studies of wave generation and the efficiency of non-wave (reconnection) mechanisms are completed. The most challenging task will be to incorporate a reconnection heating mechanism into the models. The PI's resulting models will then be used to predict activity in the solar chromosphere, transition region, and coronal holes. By comparing these predictions with solar observational data, the PI will be able to determine the basic heating and wind acceleration mechanisms operating in different regions of the solar atmosphere.The proposed research will play an important role in ongoing efforts to understand the principal energy sources of the solar atmosphere and the basic physical processes responsible for creating the heliosphere. The PI plans a public outreach program centered on several planetarium shows devoted to the Sun, and presented to students and the general public in a new campus facility.

在NSF的支持下，PI已经建立了太阳色球层的理论模型。他确定了声波是非磁性区域的加热源，纵向和横向管波是磁通管的加热源；声波和电磁波都在太阳对流区产生。PI的主要结论是，光靠引力波无法提供足够的能量来解释在最上层色球层、太阳过渡区和日冕中观测到的所有活动。他还建立了基于磁波动量沉积的太阳风理论模型，他发现这些磁波对背景介质施加的力对太阳风的加速有重要贡献。确定太阳大气中的加热机制和解释由这种加热引起的太阳活动是太阳物理研究中的重要问题，也是尚未解决的问题。PI建议通过开发一种新方法来解决这些问题，该方法允许他构建模型来描述整个太阳大气并解释大气振荡。所提出的模型将是理论性的、自洽的和时间相关的，并且将在完成对波的产生和非波（重连）机制的效率的全面研究之后构建。最具挑战性的任务将是在模型中加入重连加热机制。PI的结果模型将用于预测太阳色球层、过渡区和日冕洞的活动。通过将这些预测与太阳观测数据进行比较，PI将能够确定在太阳大气不同区域运行的基本加热和风加速机制。拟议的研究将在持续努力中发挥重要作用，以了解太阳大气的主要能量来源和产生日球层的基本物理过程。PI计划在一个新的校园设施中向学生和公众展示几场以太阳为中心的天文馆展览。