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Solar Flare Gamma Ray and Neutron Studies

太阳耀斑伽马射线和中子研究

基本信息

批准号：
8717676
负责人：
Richard Lingenfelter
金额：
$ 10.99万
依托单位：
University of California-San Diego
依托单位国家：
美国
项目类别：
Continuing Grant
财政年份：
1987
资助国家：
美国
起止时间：
1987-12-01 至 1990-05-31
项目状态：
已结题

来源：
https://www.nsf.gov/awardsearch/showAward?AWD_ID=8717676&HistoricalAwards=false
关键词：
Solar Flare Gamma Ray Neutron

项目摘要

Observations of neutron and gamma-ray-line emission from solar flares are providing important new information on particle acceleration in solar flares and on the flare process itself. These gamma-rays and neutrons are produced directly by nuclear interactions of the flare-accelerated protons and heavier ions with ambient gas in the solar atmosphere. Thus they yield the most direct information available on the total number, energy spectrum, time dependence, and angular distribution of the accelerated ions in the flare region, and they can provide unique new information on both the scale height and the 3He/H ratio in the solar photosphere. Gamma ray line emission was first observed in 1973 and relativistic neutrons were observed in 1983. These observations have stimulated much more extensive theoretical calculations of gamma-ray line and neutron production by flare particle interactions and comparison of the flare observations with these calculations have provided much important new information. This grant will pursue these general theoretical objectives. In particular, the PI will calculate the gamma ray line emission with a view to determining the time dependence of particle acceleration in flares. All of this is with a view to comparing theory with observations in order to narrow the field of candidate models of solar flares.

对太阳耀斑中子和伽马射线线发射的观测为太阳耀斑中的粒子加速和耀斑过程本身提供了重要的新信息。这些伽马射线和中子是由耀斑加速的质子和较重的离子与太阳大气中的环境气体的核相互作用直接产生的。因此，它们可以提供有关耀斑区域中加速离子的总数、能谱、时间依赖性和角度分布的最直接信息，并且可以提供有关太阳光球层中的尺度高度和 3He/H 比的独特新信息。伽马射线线发射于 1973 年首次被观测到，相对论性中子于 1983 年被观测到。这些观测激发了对耀斑粒子相互作用产生伽马射线和中子的更广泛的理论计算，并且耀斑观测与这些计算的比较提供了许多重要的新信息。这笔赠款将致力于实现这些一般理论目标。特别是，PI 将计算伽马射线线发射，以确定耀斑中粒子加速度的时间依赖性。所有这些都是为了将理论与观测进行比较，以缩小太阳耀斑候选模型的范围。