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.

主要研究者（PI）将研究太阳和地球附近太阳风中的不连续性，并使用这些结构研究太阳下的磁重新连接事件。 他的团队将分类不连续性类型，计算不连续性的发生频率是太阳风特征和太阳源区域的函数，并开发出预测到达地球的血浆结构的类型。 PI的团队将统计地分析来自风，ACE，Helios-1和Helios-2航天器的高分辨率等离子体和磁场数据，以制定标准以识别太阳风中现有的各种类型的不连续性。 然后，团队将使用Wang-Sheeley-Arge（WSA）模型将L1处的太阳风映射回太阳能表面，从而确定从哪种类型的太阳能表面区域（例如，冠状孔，冠状孔，小冠状孔或活性区域的冠状孔中心或活性区域）各自的目录起源于目录中。使用其不连续性目录，PI的团队将识别血浆边界和上电子边界，然后使用磁场和1 AU收集的等离子数据计算每个边界对之间的磁通量。 从太阳风的通量和计算出的运输时间中，将估算太阳面上的重新连接速率。该项目所需的数据可在线访问。 PI期望这种努力能够更好地理解气压层中血浆结构的起源以及在太阳风中作用的物理过程。 该项目将培训博士后科学家，研究结果将纳入一个教育外展计划中。