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.

在1970年代末和1980年代初期，发起了两个卫星实验，以测量太阳辐照度，有时称为“太阳常数”。 这两个卫星实验已经很清楚地表明，太阳辐照度的时间尺度从几分钟到几年。 最大的振幅变化发生在5到7天的时间尺度上，并且显然与大黑子基团穿过太阳的表面相关。 具有讽刺意味的是，太阳辐照度的最高值是在太阳周期的峰值期间，当时太阳斑的平均面积比其他时间大得多。 太阳能最大值附近的增强辐照度可能是由于大面积的面积，在肢体附近的白光中看到的磁场区域，因为认为明亮的斑块太微弱了，太稀缺了，无法与日光浴相比会导致太阳辐照度的显着变化。 在过去的六年中，SFO的工作表明，Faculae确实是发射的重要来源。 特别是，在1982年，一组大日光浴的人表明，Faculae的发射大致平衡了黑子的阻塞。 散布在太阳上的磁场的碎片（所谓的光电网络的一部分）可能是导致在太阳能最大值时看到的发射盈余。 通过在各种波长下获得太阳的准确光度图像，它旨在确定卫星辐照度监测器测量中的黑子，faculae和网络的影响，并允许搜索更加微妙的太阳效应。 这项工作的结果可能有助于更好地预测太阳能磁性周期对地球气候的影响。