1.2 Other indicators of solar activity

Reconstructions of R prior to the early 19th century are increasingly uncertain. In order to tackle problems related to sporadic and often unreliable observations, Hoyt and Schatten (1998) introduced the Group Sunspot Number (GSN) as an alternative indicator of solar activity. In contrast to RW, the GSN only relies on counts of sunspot groups as a more robust indicator, disregarding the number of spots in each group. Furthermore, while RW is determined for any given day from a single observer’s measurements (a hierarchy of secondary observers is defined for the case if data from the primary observer were unavailable), the GSN uses a weighted average of all observations available for a given day. The GSN series has been reproduced for the whole period 1611 – 1998 (Figure 1View Image) and it is generally agreed that for the period 1611 – 1818 it is a more reliable reconstruction of solar activity than the relative sunspot number. Yet there have been relatively few attempts to date to use this data series for solar cycle prediction. One factor in this could be the lack of regular updates of the GSN series, i.e., the unavailability of precise GSN values for the past decade.
View Image

Figure 1: 13-month sliding averages of the monthly average relative sunspot numbers R (green) and group sunspot numbers RG (black) for the period 1611 – 1998.

Instead of the sunspot number, the total area of all spots observed on the solar disk might seem to be a less arbitrary measure of solar activity. However, these data have been available since 1874 only, covering a much shorter period of time than the sunspot number data. In addition, the determination of sunspot areas, especially farther from disk center, is not as trivial as it may seem, resulting in significant random and systematic errors in the area determinations. Area measurements performed in two different observatories often show discrepancies reaching ∼ 30% for smaller spots (cf. the figure and discussion in Appendix A of Petrovay et al., 1999).

A number of other direct indicators of solar activity have become available from the 20th century. These include, e.g., various plage indices or the 10.7 cm solar radio flux – the latter is considered a particularly good and simple to measure indicator of global activity (see Figure 2View Image). As, however, these data sets only cover a few solar cycles, their impact on solar cycle prediction has been minimal.

View Image

Figure 2: Monthly values of the 10.7 cm radio flux in solar flux units for the period 1947 – 2009. The solar flux unit is defined as 10–22 W/m2 Hz. The green curve shows Rm + 60, where Rm is the monthly mean relative sunspot number. (The vertical shift is for better comparison.) Data are from the NRC Canada (Ottawa/Penticton).

Of more importance are proxy indicators such as geomagnetic indices (the most widely used of which is the aa index), the occurrence frequency of aurorae or the abundances of cosmogenic radionuclides such as 14C and 10Be. For solar cycle prediction uses such data sets need to have a sufficiently high temporal resolution to reflect individual 11-year cycles. For the geomagnetic indices such data have been available since 1868, while an annual 10Be series covering 600 years has been published very recently by Berggren et al. (2009). Attempts have been made to reconstruct the epochs and even amplitudes of solar maxima during the past two millennia from oriental naked eye sunspot records and from auroral observations (Stephenson and Wolfendale, 1988Nagovitsyn, 1997Jump To The Next Citation Point), but these reconstructions are currently subject to too many uncertainties to serve as a basis for predictions. Isotopic data with lower temporal resolution are now available for up to 50 000 years in the past; while such data do not show individual Schwabe cycles, they are still useful for the study of long term variations in cycle amplitude. Inferring solar activity parameters from such proxy data is generally not straightforward.

  Go to previous page Go up Go to next page