Group Sunspot Numbers: A new solar activity reconstruction
Group Sunspot Numbers: A new solar activity reconstruction
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DOI：
10.1023/a:1005056326158
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发表时间：
1998-08-01
期刊：
影响因子：
2.8
通讯作者：
Schatten, KH
中科院分区：
文献类型：
--
作者：
Hoyt, DV;Schatten, KH
在本文中，我们构建了一个时间序列称为太阳黑子群数。太阳黑子群数被设计成内部更加自洽（即，更少依赖于看到最微小的斑点）和更少的噪音比狼太阳黑子数。它使用观测到的太阳黑子群的数量，而不是太阳黑子群和单个太阳黑子。每日、每月和每年的平均值来自1610年至今。太阳黑子群数使用了沃尔夫在1874年之前没有使用的117个观测者的65941个观测数据。因此，我们计算了1610-1995年111358天的太阳活动日值，而沃尔夫太阳黑子数为66168天。太阳黑子群的数字也有其随机和系统误差的估计表。太阳黑子群数的产生和初步分析使我们得出几个结论：（1）1882年以前的太阳活动比一般认为的要低，因此最近几十年的太阳活动比几个世纪以来的要高。(2)在1801年而不是1805年有一个太阳活动高峰，所以没有像沃尔夫太阳黑子数报告的那样17年的长异常周期。现在最长的周期不超过15年。(3)沃尔夫太阳黑子数有许多不均匀性，这些不均匀性来自观测者的噪声，这种噪声影响了日、月和年的平均值。太阳黑子群数也有观测者噪声，但它比沃尔夫太阳黑子数中的噪声要小得多。太阳黑子群数的设计与沃尔夫太阳黑子数相似，但是，即使两个指数都有完美的输入，也会有一些差异，主要是在日值上。
In this paper, we construct a time series known as the Group Sunspot Number. The Group Sunspot Number is designed to be more internally self-consistent (i.e., less dependent upon seeing the tiniest spots) and less noisy than the Wolf Sunspot Number. It uses the number of sunspot groups observed, rather than groups and individual sunspots. Daily, monthly, and yearly means are derived from 1610 to the present. The Group Sunspot Numbers use 65 941 observations from 117 observers active before 1874 that were not used by Wolf in constructing his time series. Hence, we have calculated daily values of solar activity on 111 358 days for 1610-1995, compared to 66 168 days for the Wolf Sunspot Numbers. The Group Sunspot Numbers also have estimates of their random and systematic errors tabulated. The generation and preliminary analysis of the Group Sunspot Numbers allow us to make several conclusions: (1) Solar activity before 1882 is lower than generally assumed and consequently solar activity in the last few decades is higher than it has been for several centuries. (2) There was a solar activity peak in 1801 and not 1805 so there is no long anomalous cycle of 17 years as reported in the Wolf Sunspot Numbers. The longest cycle now lasts no more than 15 years. (3) The Wolf Sunspot Numbers have many inhomogeneities in them arising from observer noise and this noise affects the daily, monthly, and yearly means. The Group Sunspot Numbers also have observer noise, but it is considerably less than the noise in the Wolf Sunspot Numbers. The Group Sunspot Number is designed to be similar to the Wolf Sunspot Number, but, even if both indices had perfect inputs, some differences are expected, primarily in the daily values.