Collaborative Research: SHINE--Stochastic Particle Acceleration by Turbulence in Solar Flares

合作研究：SHINE——太阳耀斑中湍流的随机粒子加速

• 批准号: 0648699
• 负责人: Alexandre Lazarian
• 金额: $ 13.96万
• 依托单位: University of Wisconsin-Madison
• 依托单位国家: 美国
• 项目类别: Continuing Grant
• 财政年份: 2007
• 资助国家: 美国
• 起止时间: 2007-01-01 至 2009-12-31
• 项目状态: 已结题
• 来源: https://www.nsf.gov/awardsearch/showAward?AWD_ID=0648699&HistoricalAwards=false
• 关键词: Collaborative; Research; SHINE; Stochastic; Particle; Collaborative; Research; SHINE; Stochastic; Particle

The observed radiation from solar flares and solar energetic particles (SEPs) indicates the presence of nonthermal particles and very hot plasmas. While it is generally believed that the source of the energy is magnetic reconnection, the origin of these high energy particles is a matter of considerable debate. Based on new observations (notably high resolution data from RHESSI), the PIs have proposed that most of the energy released is initially converted into plasma turbulence, which then accelerates particles and heats the plasma further. This team thus plans to investigate the role of anisotropic turbulence cascade and damping in the acceleration of solar plasmas. They plan to use accurate dispersion relations that go beyond simple MHD treatments in their evaluation of wave-wave and wave-particle interactions. Their goal is to incorporate these results into a solar flare model to present a self-consistent picture of flares that can be tested by observations. The Stanford PI and his associates have developed numerical codes to study particle heating, acceleration, transport, and radiation. The Wisconsin Co-PI and his group have substantial expertise in the area of magnetic plasma turbulence and have developed codes for treating turbulence in the regimes relevant to the study. Recent work by the PI and his associates has shown that turbulence can explain many features of the new observations. They expect turbulence to be present in flare plasmas and their simulations confirm this. The Co-PI has also made progress in the understanding of compressible MHD turbulence. This Stanford-Wisconsin team thus believes that incorporating the physics of turbulence generation and evolution, and its coupling with solar plasma, will now permit advances in solar flare modeling. The complementary expertise of the Stanford and Wisconsin PIs could provide the tools necessary for a breakthrough in this important problem. This research is expected to have a strong educational aspect by involving not only postdoctoral fellows and graduate students at both institutions, but also undergraduate students. The results of this research will be presented at local educational and public institutions through the auspices of Stanford's Haas Center for Public Service.

来自太阳耀斑和太阳能颗粒（SEP）的观察到的辐射表明存在非热颗粒和非常热的等离子体。 虽然通常认为能量的来源是磁重新连接，但这些高能量颗粒的起源是一个很大的争论。 基于新的观察结果（尤其是Rhessi的高分辨率数据），PI提出，释放的大多数能量最初被转化为血浆湍流，然后加速颗粒并进一步加热血浆。 因此，该团队计划调查各向异性湍流级联和阻尼在太阳等离子体加速中的作用。 他们计划使用准确的分散关系，这些关系在评估波浪和波粒相互作用时超越了简单的MHD处理。 他们的目标是将这些结果纳入太阳耀斑模型中，以呈现可以通过观察结果测试的耀斑的自一致图片。斯坦福PI和他的同事开发了数值代码来研究颗粒加热，加速，运输和辐射。 威斯康星州的Co-Pi及其小组在磁等离子体湍流领域具有丰富的专业知识，并开发了与研究相关的制度中处理湍流的代码。 PI和他的同事最近的工作表明，湍流可以解释新观察的许多特征。 他们希望在耀斑等离子体中存在湍流，他们的模拟证实了这一点。 CO-PI在理解可压缩的MHD湍流方面也取得了进展。 因此，这支斯坦福 - 威斯康星州的团队认为，将湍流产生和进化的物理学及其与太阳等离子体结合在一起，现在将允许在太阳耀斑建模中进步。 斯坦福大学和威斯康星州PI的互补专业知识可以提供突破这一重要问题所需的工具。预计这项研究将具有强大的教育方面，不仅涉及两家机构的博士后研究员和研究生，而且还涉及本科生。 这项研究的结果将通过斯坦福HAAS公共服务中心的主持在当地的教育和公共机构中呈现。