Solar cycle variations in solar and interplanetary ions observed with Interplanetary Monitoring Platform 8
Solar cycle variations in solar and interplanetary ions observed with Interplanetary Monitoring Platform 8
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使用行星际监测平台 8 观测到的太阳和行星际离子的太阳周期变化
DOI：
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发表时间：
2004
期刊：
影响因子：
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通讯作者：
T. Armstrong
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文献类型：
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作者：
K. Simunac;T. Armstrong
[1]高能质子（0.39-440 MeV），α粒子（0.59-52 MeV/核子）和中等核（碳，氮和氧; 0.7-8.8 MeV/核子）已被行星际监测平台8号（IMP 8）航天器上的带电粒子测量实验（CPME）从1973年至今观测到。我们总结了1973年10月至2000年11月期间获得的结果，超过两个完整的太阳周期。我们相信，这些对太阳和行星际粒子的观测是迄今为止从单一仪器获得的最长的观测。人为因素已经被小心地从这个数据集中删除，包括由于1989年电子反符合屏蔽失败而导致的背景变化。我们计算了单个太阳周期的平均值，以及27年期间所看到的一切的“大”平均值。质子、α粒子和中等核的“大”平均能谱可以用总能量的幂律函数来描述，其指数为−2，其中E的单位是MeV，通量是粒子/（cm 2 s sr MeV）。计算了太阳活动最小（H/He = 30; He/medium = 95）和最大（H/He = 61; He/medium = 45）时相同速度下高能核的组分丰度比。我们还考虑了太阳黑子数和行星际粒子通量之间可能的关系，使用各种平均间隔和时间滞后和铅，但没有发现任何结果，可用于预测粒子通量从太阳黑子数在短时间间隔（通常是几个太阳旋转）。
[1] Energetic protons (0.39–440 MeV), alpha particles (0.59–52 MeV/nucleon), and medium nuclei (carbon, nitrogen, and oxygen; 0.7–8.8 MeV/nucleon) have been observed with the Charged Particle Measurement Experiment (CPME) aboard the Interplanetary Monitoring Platform 8 (IMP 8) spacecraft from 1973 to the present. We summarize the results obtained for the period October 1973 through November 2000, more than two complete solar cycles. We believe that these observations of solar and interplanetary particles are the longest set from a single instrument yet obtained. Artifacts have been carefully removed from this data set, including background changes due to the failure in 1989 of an electronic anticoincidence shield. We have computed averages over individual solar cycles as well as “grand” averages of everything seen over the 27-year period. The “grand” average energy spectrum of protons, alphas, and medium nuclei is well described by a power law function in total energy with exponent −2, where E is in units of MeV total energy and flux is particles/(cm2 s sr MeV). Compositional abundance ratios for energetic nuclei at the same speeds are calculated for times of minimum (H/He = 30; He/medium = 95) and maximum (H/He = 61; He/medium = 45) solar activity. We also considered possible relationships between sunspot number and interplanetary particle flux using a variety of averaging intervals and time lags and leads but found no result that could be used to predict particle fluxes from sunspot numbers over short intervals (typically several solar rotations).