Mysterious Activities of Our Magnificent Sun

在先前NSF的支持下，PI已经构建了太阳色球层的理论模型。他发现声波是非磁性区域的热源，而纵向和横向管波是磁通量管的热源;声波和磁波都是在太阳对流区产生的。PI的主要结论是，光靠波无法提供足够的能量来解释色球层最上层、太阳过渡区和日冕中观察到的所有活动。他还建立了基于磁波动量沉积的太阳风理论模型，并发现这些磁波对背景介质施加的力对太阳风的加速有很大贡献。确定太阳大气中的加热机制，并解释由这种加热导致的太阳活动，是太阳物理学研究中重要而尚未解决的问题。PI建议通过开发一种新的方法来解决这些问题，使他能够构建模型来描述整个太阳大气层并解释大气振荡。所提出的模型将是理论的，自洽的，和时间相关的，它们将被构建后，波的产生和效率的非波（重联）机制的全面研究完成。最具挑战性的任务将是将重连加热机制纳入模型。PI的最终模型将用于预测太阳色球层、过渡区和冕洞的活动。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，拟议的研究将在不断努力了解太阳大气的主要能源和负责创建日光层的基本物理过程中发挥重要作用。PI计划以几个天文馆展示太阳为中心的公共宣传计划，并在新的校园设施中向学生和公众展示。

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.