RUI: A Proposal for the Collection ad Analysis of Photometric Data Giving Solar Irradiance Fluctuations

RUI：收集和分析太阳辐照度波动的光度数据的提案

• 批准号: 8817634
• 负责人: Gary Chapman
• 金额: $ 3.61万
• 依托单位: The University Corporation, Northridge
• 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 1992-08-31
• 项目状态: 已结题
• 来源: https://www.nsf.gov/awardsearch/showAward?AWD_ID=8817634&HistoricalAwards=false
• 关键词: RUI; Proposal; Collection; ad; Analysis

In the late 1970's and early 1980's two satellite experiments were launched to measure the solar irradiance, sometimes called the "solar constant". These two satellite experiments have shown quite clearly that the solar irradiance varies on time scales from minutes to years. The largest amplitude variations occur on time scales of 5 to 7 days and are clearly associated with the passage of large sunspot groups across the face of the sun. Ironically, the highest values of solar irradiance are during the peak of the solar cycle when the average area of sun spots is much larger than at other times. The enhanced irradiance near solar maximum may be due to the presence of large areas of faculae, magnetic field regions seen in white light near the limb as bright patches were thought to be too faint and too scarce to cause a significant change in solar irradiance compared to sunspots. The work at the SFO over the last six years has shown that faculae are indeed important sources of emission. In particular, it was shown for a group of large sunspots in 1982 that the emission from faculae approximately balanced the blocking of sunspots. The fragments of magnetic fields scattered across the sun, part of what is called the photospheric network, may be responsible for the surplus of emission that is seen at the time of the solar maximum. By obtaining accurate photometric images of the sun at various wavelengths, it is intended to determine the effects of sunspots, faculae and the network in the measurements of satellite irradiance monitors and permit the search for even more subtle solar effects. The results of this work may help to better predict the effects of the solar magnetic cycle on the earth's climate.

1970年代末和1980年代初， 开始了测量太阳辐照度的实验， 有时被称为“太阳常数”。 这两颗卫星 实验已经清楚地表明， 时间尺度从几分钟到几年不等。 最大的 振幅变化发生在5至7天的时间尺度上， 与太阳黑子群的移动有关 在太阳的表面。 具有讽刺意味的是， 太阳辐射是在太阳活动周期的高峰期， 太阳黑子的平均面积比其他时候大得多。 太阳活动极大期附近的辐射增强可能是由于 存在大面积光斑，可见磁场区域 在肢体附近的白色光中， 太微弱太稀少， 与太阳黑子相比。 证券及期货条例 过去六年的研究表明光斑确实很重要 排放源。 特别是，它显示了一组 1982年的大型太阳黑子， 大致平衡了太阳黑子的阻挡。 所述片段 太阳磁场的一部分 称为光球网络，可能是负责 在太阳活动时所看到的多余的辐射 最大. 通过获得精确的太阳光度图像， 各种波长，旨在确定 太阳黑子，光斑和网络的测量， 卫星辐照度监测器，并允许搜索更多 微妙的太阳效应。 这项工作的结果可能有助于 更好地预测太阳磁周期对地球的影响， 地球的气候。