Expressions to determine temperatures and emission measures for solar X-ray events from GOES measurements
Expressions to determine temperatures and emission measures for solar X-ray events from GOES measurements
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DOI：
10.1007/bf00152409
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发表时间：
1984-08
期刊：
影响因子：
2.8
通讯作者：
R. Thomas;R. Starr;C. Crannell
中科院分区：
文献类型：
--
作者：
R. Thomas;R. Starr;C. Crannell
我们已经开发出的表达式，给出了有效的色温和相应的发射措施，观测到的太阳X射线事件的仪器上的任何GOES卫星。自1976年以来，这些卫星一直被用于连续监测两个宽波段（约0.5-4纳秒和1-8纳秒）的全太阳X射线辐射，时间分辨率为3秒。为了模拟不同等离子体温度下的太阳X射线输入，我们使用了D。L.麦肯齐这些光谱通过Donnellyet等人给出的两个GOES探测器的波长相关传递函数折叠。（1977年）。得到的检测器响应和它们的比例作为等离子体温度的函数，然后拟合简单的分析曲线。在500万度到3000万度的整个范围内，这些拟合再现了2%以内的计算色温和5%以内的计算发射测量。通过McKenzie提供的理论光谱，我们可以确定任何一对宽带X射线探测器的相似表达式，其灵敏度限制在0.2到100 nm之间的波长。
We have developed expressions which give the effective color temperatures and corresponding emission measures for solar X-ray events observed with instruments onboard any of the GOES satellites. Since 1976, these satellites have been used to monitor continuously the full-Sun X-ray emission in two broadband wavelength intervals (approximately 0.5–4 Å and 1–8 Å) with a time resolution of 3 s. To simulate the solar X-ray input at a variety of plasma temperatures, we used theoretical spectra provided by D. L. McKenzie. These spectra were folded through the wavelength dependent transfer functions for the two GOES detectors as given by Donnellyet al.(1977). The resulting detector responses and their ratio as a function of plasma temperature were then fit with simple analytic curves. Over the entire range between 5 and 30 million degrees, these fits reproduce the calculated color temperatures within 2% and the calculated emission measures within 5%. With the theoretical spectra provided by McKenzie, we can determine similar expressions for any pair of broadband X-ray detectors whose sensitivities are limited to wavelengths between 0.2 and 100 Å.