Particle Acceleration in Solar Flares

太阳耀斑中的粒子加速

• 批准号: 8909845
• 负责人: Dean Smith
• 金额: $ 10万
• 依托单位: Berkeley Research Associates Inc
• 依托单位国家: 美国
• 项目类别: Standard Grant
• 财政年份: 1989
• 资助国家: 美国
• 起止时间: 1989-09-01 至 1993-02-28
• 项目状态: 已结题
• 来源: https://www.nsf.gov/awardsearch/showAward?AWD_ID=8909845&HistoricalAwards=false
• 关键词: Particle; Acceleration; Solar; Flares

A Key problem in solar flare physics is the manner in which protons and other particles are accelerated in a few seconds as evidenced by impulsive y-ray emission. The most widely accepted models in explaining this acceleration are shock acceleration and stochastic acceleration by Alfven or magnetosonic waves. Neither of these models has developed self-consistency or has direct observational verification. This grant will permit the consistent development of a single-loop Alfven wave stochastic acceleration model as the topic most likely to allow a close interaction between theory and observations. A half-loop is divided into 3 coronal sections attached to a model chromosphere and photosphere. The coronal sections include the source where primary acceleration occurs, a section beyond the source where further acceleration occurs and a transport section in which protons propagate diffusively. Unlike previous work, it will be a complete model for nonrelativistic energies including a nuclear interaction calculation. Thus , it will be possible to study the effect of changing the spectrum and/or power of turbulence in the source, the loop size, etc., throughout the whole loop. In short, it will be possible to put the stochastic acceleration model to a very thorough test. Observational consequences in prompt y-ray emission come from the nuclear interaction part of the calculation. A radio diagnostic of the low-frequency turbulence in the source will be developed to provide an observational means of verifying its existence. These results will increase understanding in this important area of research. The overall aim is to improve current understanding of particle acceleration at the sun. These particles form part of the earth's environment and, therefore, this work is important to S/T relations. //

太阳耀斑物理学的一个关键问题是 质子和其他粒子在几秒钟内被加速， 由脉冲γ射线辐射证实 最广泛接受的 解释这种加速度的模型是冲击加速度， 阿尔文波或磁声波的随机加速。 这两种模式都没有发展出自我一致性， 有直接的观测验证。 这笔赠款将允许 单圈Alfven波一致发展 随机加速模型作为最有可能允许 理论与观察之间的密切互动。 半环 分为3个冠状部分，连接到模型上 色球和光球。 冠状面包括 主加速发生的地方， 发生进一步加速的源和传输部分 其中质子扩散地传播。 与以前的工作不同， 将是一个完整的非相对论能量模型，包括 核相互作用计算 因此，将有可能 研究改变频谱和/或功率的影响 源中的湍流、环路大小等，在整个 整个循环 简而言之，将随机 加速度模型进行了非常彻底的测试。 观测到的瞬发γ射线辐射的结果 从核相互作用的计算部分。 无线电 对源中低频湍流的诊断将是 开发的目的是提供一种观测手段， 存在 这些结果将增加对这一问题的理解。 重要的研究领域。 总体目标是改善 目前对太阳粒子加速的理解。 这些 粒子构成了地球环境的一部分，因此， 这项工作对科技关系具有重要意义。 //