SHINE: Origin and Evolution of Structure in the Solar Wind

SHINE：太阳风结构的起源和演化

• 批准号: 0852150
• 负责人: Joseph Borovsky
• 金额: $ 36.01万
• 依托单位: Department of Energy Albuquerque Operations Office
• 依托单位国家: 美国
• 项目类别: Interagency Agreement
• 财政年份: 2009
• 资助国家: 美国
• 起止时间: 2009-09-01 至 2013-08-31
• 项目状态: 已结题
• 来源: https://www.nsf.gov/awardsearch/showAward?AWD_ID=0852150&HistoricalAwards=false
• 关键词: SHINE; Origin; Evolution; Structure; Solar

The Principal Investigator (PI) will investigate discontinuities in the solar wind near the Sun and at the Earth, and use these structures to study magnetic reconnection events at the Sun. His team will catalog discontinuity types, calculate discontinuity occurrence frequency as a function of solar wind characteristics and solar source region, and develop a capability to predict the types of plasma structures that arrive at Earth. The PI's team will statistically analyze high-resolution plasma and magnetic field data from the Wind, ACE, Helios-1, and Helios-2 spacecraft to develop criteria to identify the various types of discontinuities existing in the solar wind. The team will then use the Wang-Sheeley-Arge (WSA) model to map the solar wind at L1 back to the solar surface, and thus determine from which type of solar-surface region (for example, center of coronal hole, coronal-hole edge, small coronal hole, or active region) each discontinuity in their catalog originated. Using their discontinuity catalog, the PI's team will identify plasma boundaries and suprathermal-electron boundaries, and then calculate the amount of magnetic flux between each boundary pair using magnetic field and plasma data collected at 1 AU. From this amount of flux and the calculated transit time of the solar wind, the will estimate the reconnection rate at the solar surface.The data needed for this project are accessible online. The PI expects this effort to lead to a better understanding of the origin of plasma structure in the heliosphere and the physical processes acting in the solar wind. This project will train a postdoctoral scientist and the research results will be incorporated into an educational outreach program.

首席研究员（PI）将研究太阳附近和地球上太阳风的不连续性，并利用这些结构来研究太阳的磁重联事件。 他的团队将对不连续性类型进行分类，计算作为太阳风特征和太阳源区域函数的不连续性发生频率，并开发预测到达地球的等离子体结构类型的能力。 PI 的团队将对 Wind、ACE、Helios-1 和 Helios-2 航天器的高分辨率等离子体和磁场数据进行统计分析，以制定标准来识别太阳风中存在的各种类型的不连续性。 然后，该团队将使用 Wang-Sheeley-Arge (WSA) 模型将 L1 处的太阳风映射回太阳表面，从而确定其目录中的每个不连续性源自哪种类型的太阳表面区域（例如日冕洞中心、日冕洞边缘、小日冕洞或活动区域）。使用他们的不连续性目录，PI 团队将识别等离子体边界和超热电子边界，然后使用以 1 AU 收集的磁场和等离子体数据计算每个边界对之间的磁通量。 根据该通量和计算出的太阳风传输时间，将估计太阳表面的重新连接率。该项目所需的数据可在线获取。 PI 预计这项工作将有助于更好地了解日光层中等离子体结构的起源以及太阳风中的物理过程。 该项目将培养一名博士后科学家，研究成果将纳入教育推广计划。