# Sunspot Observations of Rudolf Wolf from 1849 – 1893

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## Abstract

The sunspot observations of Rudolf Wolf form the core of the Wolf series of sunspot relative numbers, or Wolf numbers, since his observations define the original scale of the series and also the main course of solar activity from 1849 to 1893. Unfortunately, the raw data for the years 1856 to 1869 were never published in full detail. The heritage group of the Rudolf Wolf Society in Switzerland digitized parts of the hitherto unpublished original source book of the Wolf series and put it on its website www.wolfinstitute.ch . Now, the Wolf numbers from 1849 to 1876, as provided by the World Data Center for Solar Index and Long-term Solar Observations (WDC-SILSO), can be reconstructed in every detail, since the source book contains all the raw sunspot group and individual spot numbers as well as the implemented calibration and interpolation methods. Thus, the observations made by Rudolf Wolf with the 83/1320 mm Fraunhofer refractor and with the 40/700 mm Parisian refractor as well as those made by Heinrich Schwabe can be identified and separated now. In this article, we describe Wolf’s instruments and methods of observation. An inspection of the source book and other published sources reveals that the calibration factor of the 40/700 mm Parisian refractor should probably be lowered. Since no appropriate comparison observations are available, the scale transfer from Heinrich Schwabe to Rudolf Wolf has to be analyzed further.

### Keywords

Solar cycle Observations Sunspots Statistics## 1 Introduction

Homogeneity is considered as the most important property of the Wolf series since without a stable scale no valid conclusions about variations in the long-term course of the solar activity can be drawn. A homogenization of the Wolf series should be based on a fully transparent reconstruction of the daily Wolf numbers as provided by WDC-SILSO version 1.0 (Friedli 2009). But since the original raw data and the data-reduction methods were never published, a thorough homogeneity testing and an appropriate correction of the Wolf series seems up to now nearly impossible (Clette *et al.* 2015).

Based on some hitherto unpublished sources from the archives of the former Swiss Federal Observatory in Zurich we reconstruct in this article the daily raw observations of Rudolf Wolf, including the number of sunspot groups and the number of individual spots. His observations form the core of the Wolf series since they define the original scale of the series and the main course of solar activity from 1849 to 1893. But, unfortunately, it was widely neglected that Rudolf Wolf changed his standard instrument two times and that he suffered from an eyesight diminishment in his later years, although Wolf (1894) and Wolfer (1895) had claimed that the Wolf series had to be recalculated.

In Section 2 we give some historical background information on Wolf’s sunspot observations and a description of his main instruments. In Section 3 we review the newly digitized raw observations of the Wolf series from 1849 to 1876. In Section 4 we give some historical background information concerning Wolf’s method of counting sunspot groups and individual spots and on the eyesight diminishing in his later years. In Section 5 we review Wolf’s estimates of the \(k\)-factor of his smaller instrument and of the observations of Heinrich Schwabe. In Section 6 the conclusions are summarized.

## 2 Historical Outline

### 2.1 First Attempts in Berne

*Notices*, Wolf summarized his findings and concluded that there would be no quick progress in the exploration of the physical nature of the spots and that it would be better to collect more observations (Wolf 1849b). In January 1849, Wolf started a systematic observing program with daily determinations of the number of sunspot groups and individual spots (Wolf 1850). Only some years later, Wolf noticed that the frequency of sunspots had markedly diminished since his first observations in 1847 and 1848 and he introduced in 1850 a first version of so-called sunspot relative numbers, or Wolf numbers, to quantify this effect (Wolf, 1851; Friedli and Keller, 1993).

### 2.2 The Standard Refractor of the Wolf Series

Rudolf Wolf made most of his sunspot observations with a refractor fabricated by Utzschneider and Fraunhofer in Munich, which belonged to the Realschule (a private college focused on exact and natural sciences), where he worked as a teacher of mathematics and physics. The instrument had been acquired during the late 1820s by the well-known geologist Bernhard Studer (1794 – 1887), who became director of the Realschule during Wolf’s stay in Berne. As indicated on page 170 of Wolf (1848) the refractor had an aperture of 37 Parisian lines, a focus length of 48 Parisian inches, and eyepieces for 64- and 144-fold magnification. These dimensions match perfectly with the entry number 10 in the catalog of Utzschneider (1829). If we assume the Parisian line to equal 2.2558 mm and the Parisian inch to equal 2.7070 cm, the refractor had an aperture of 83 mm and a focal length of 1300 mm. The latter is confirmed on page 5 of Wolf (1849a), where Wolf reports a focal length of 1313 mm. The instrument was equipped with a colored glass filter for solar observations. Nothing is known about the mounting of the telescope, but in 1854 Wolf put the refractor into the dome of the newly erected tower of the observatory, where the instrument was installed on an equatorial mount designed by himself (Wolf, 1854, 1879; Flury 1929). After Wolf’s departure to Zurich, this instrument remained in Berne and was further used by Wolf’s former pupil Emil Jenzer for sunspot observations during the years 1861 to 1864 (Wolf, 1862, 1863, 1864, 1865). Later on, it was forgotten and Flury (1929), who visited the observatory in April 1925, found it completely corroded. Thus, the instrument indeed had a metallic tube, as described by Utzschneider (1829). Its further fate is unknown.

### 2.3 From Berne to Zurich

In 1855, Wolf was appointed professor of mathematics and physics at the college in Zurich, professor of astronomy and head librarian at the newly founded Federal Institute of Technology, and director of the observatory in Zurich as well. The exact date of the relocation is not known, but from the preserved letters we learn that it is almost certain that Wolf moved in the early days of August (Jaeggli, 1968; Gossweiler, 1996a, 1996b).

*et al.*1998). Wolf never used it again. Henceforth, it was part of the daily duties of Wolf’s assistants to count the groups and spots at the standard refractor. In the subsequent years, most probably in early 1870, a polarizing helioscope from G. and S. Merz was installed (Figure 3), which improved the quality of the image considerably and reduced the \(k\)-factor of the observing assistant Gustav Adolf Meyer by 15 % (Wolf 1878a). Beginning in 1876, Alfred Wolfer revived the standard instrument and from 1894 on all group and spot counts of the Wolf series were again calibrated to the original scale of this instrument. In 1962 the telescope was moved on top of the roof of the Swiss Federal Observatory. After the closure of the observing station in December 1995, the instrument was relocated by the author to the Bernese outskirts where it is still used for the daily determination of the Wolf number (Friedli, 2012, 2014, 2015).

### 2.4 Portable Telescopes

## 3 Reconstruction of the Original Observations

At first glance, virtually all of Wolf’s original observations seem to have already been published in one of the many articles in the periodicals of which he was the editor. However, if we compare the published observations with the benchmark publication of Waldmeier (1961), which for the first time contained also the daily values of the Wolf series, we find that the tables of Wolf (1856) containing the observations from 1849 to 1855 make no distinction between Wolf’s observations and those by Schwabe, and those made at the standard refractor and the Parisian refractor, either. Furthermore, no daily values of the Wolf number are given and no \(k\)-factors for reducing them to the standard scale, either. Obviously, the tables of Wolf (1856) are missing several values, whereas the year 1849 of Waldmeier (1961) is complete.

During the Bernese period, Wolf published his results regularly in the *Notices of the Bernese Society of Natural Sciences* (Graf 1894). After 1855, Wolf completed his own series with counts from other observers, but in the published tables, he did not always specify the observer. Under these circumstances, a thorough reconstruction of the combined series is not possible. In 1873, Wolf realized the importance of an explicit publication of all raw data (Wolf 1873). But although most of the original observations included in the Wolf series were published later, his own observations between July 1855 and December 1869 remained partially unknown. A further exception concerns Heinrich Schwabe, from whom he never received all of the available raw data. It seems that Wolf had to ask Schwabe at the end of each year for those observations falling within the gaps of his own series. Thus, typically no observations were available for comparison and Wolf had some difficulties in calculating a reliable calibration factor for Schwabe’s observations. During the years 1874 to 1876, Wolf recalculated the whole series backwards to 1749 and included observations from additional observers. Unfortunately, this final compilation was never published.

Among the treasures preserved in the archives of the Swiss Federal Observatory a manuscript was found containing the daily raw data for the whole Wolf series from 1610 up to 1876 (Wolf 1878a). Since Wolf considered himself as the standard observer of the series, we find all of his observations with the 83/1320 mm Fraunhofer refractor in the source book. Others, among them all of the comparison observations between the standard refractor and the Parisian instrument during the years 1860 and 1862, are irretrievably lost.

*e.g.*during the first half of December 1849. These gaps were all numerically interpolated, which can be visually explored by consulting the dynamic graph on the web site. The observer labels for the interpolated days are simply placeholders. Note that the source book mentions additional observers for this year – Schmidt and Colla – who were not known in 1856 (see Figure 6).

The source book ends in 1877, since Wolf changed the data, reduction procedure (Wolf 1878b). Now, the Wolf series no longer consisted of one single observation per day, as before, but contained the average Wolf number of several observers for some days without group numbers and individual spot numbers of the standard observer, which could no longer be handled in the form of a diary. So, Wolf published all of the raw data *in extenso* in the *Astronomische Mittheilungen*. The heritage group of the Rudolf Wolf Society digitized from these sources Wolf’s remaining observations up to 1893 and placed them on the site www.wolfinstitute.ch . Thus, all surviving daily group numbers and individual spot numbers of Rudolf Wolf as used in the published Wolf series from 1849 to 1893 are now explicitly known.

## 4 Methods of Observation

The original raw observations of Rudolf Wolf are lost, but it may easily be concluded from his articles that Wolf logged his observations in a diary – at least at the beginning. In his first report on sunspot observations, he mentioned such a notebook (Wolf 1848). Furthermore he gave observational details that could not have been provided from memory. It seems that Wolf made also some sort of sketch, since he mentioned where on the solar disk new sunspot groups appeared. The notebooks were also mentioned later on (Wolf, 1849a, 1852, 1857). However, it seems that Wolf had a somehow different observation technique than the following standard observers: Wolfer, Brunner, Waldmeier, Zelenka, and Keller. He first counted the groups and then all individual spots within the groups. This technique allowed Wolf to work fast and to use days with bad weather conditions, where only the group number could be determined. But such an approach leads to counting errors in the number of individual spots, because during maximum activity it is quite probable that the observer loses track and counts the same spots or even the same groups several times or never. To avoid such errors, the subsequent standard observers wrote the number of individual spots for each group on their approximate position within a circle drawn on a piece of scrap paper. Therefore, the number of spots could be summarized later. Since 1996, the author’s daily observation record at the 83/1320 mm Fraunhofer refractor contains a sketch of each sunspot group and several indices including the number of individual spots and the modified McIntosh classification (Friedli 2013).

Wolf was a very talented observer with a long measuring experience in geodesy, meteorology, and astronomy. However, he was nearsighted, especially in his right eye. Although there exists no portrait of Wolf wearing glasses, we learn from his diary that Wolf got a prescription during his stay in Vienna in 1838 and bought a pair of glasses from Ploessl (Larcher 1993). Also, it seems that Wolf did not see the smallest spots since his pupil and successor at the observatory of Berne, Emil Jenzer, had a \(k\)-factor of 0.85 with the same instrument and the same magnification (Wolf 1878a). During his later years Wolf’s eyesight obviously diminished (Wolfer 1895). To compensate for the loss, Wolf changed his main instrument to a more powerful instrument in 1890 (Wolf 1889).

## 5 Scale Transfer

The observations of Rudolf Wolf made with the 83/1320 mm Fraunhofer refractor in Berne and Zurich from 1849 to 1863 form the core of the Wolf series and define its scale. Wolf transferred this scale to his 40/700 mm Parisian refractor and continued the series up to 1893. Backwards in time the scale was transferred to Heinrich Schwabe. The implementation of both transfers is closely related with the invention of the \(k\)-factor. During the Bernese period Wolf published his own observations only. However, after the movement to Zurich, Wolf began to complete his series with observations from Heinrich Schwabe. Based on the experiences that Wolf gained during his educational visit to several observatories in Germany in Autumn 1851, Wolf first considered the observations by Schwabe as equivalent with his own (Wolf 1852). In 1859, Wolf discovered, based on observations by Schwabe from the years 1835 to 1850, a linear relationship between the Wolf numbers and the diurnal variations in arcminutes of the magnetic-needle (Wolf 1859). In the following year Wolf noticed that the observed values of the magnetic needle variations were different from the predicted ones and thus, the scale of the combined Wolf number series had changed since 1850 (Wolf 1860). As a quick fix, Wolf added a calibration factor [\(k\)] in the formula of the Wolf number (Wolf 1861). To estimate the \(k\)-factor values, he made in 1860 with the Parisian refractor 109 comparison observations and deduced a \(k\)-factor of 1.5 (Wolf 1861). In 1861 and 1862 Wolf made some additional 26 and 120 comparison observations and found values for \(k\) of 1.43 and 1.45, respectively, slightly lower than before (Wolf, 1862, 1863). Finally, he adopted 1.5 (Wolf 1878a). If we calculate a weighted average of the above values, excluding some 49 less-reliable indirect comparisons with other observers during the year 1860, we find \(k\) = 1.44. Thus, it seems that the \(k\)-factor for the 40/700 mm Parisian refractor as fixed by Wolf (1878a) is probably too high and should be lowered. But this has to be analyzed further.

Interestingly, Wolf did not adapt his \(k\)-factor when he replaced his beloved 40/700 mm Parisian refractor with the 42/800 mm Fraunhofer refractor in 1890.

The reconstruction of the transfer from Wolf to Schwabe is more complicated since it seems that Wolf received from Schwabe only counts from those observations lying in the gaps of his own series. Thus, the value of \(k\) = 1.25 as given by Wolf (1878a), is quite unreliable, since no comparison observations were available and Wolf had to calculate Schwabe’s \(k\)-factor via secondary observers (Wolf, 1861, 1862). Furthermore, it remains questionable if the same value should also be applied to the years before 1849 since the Wolf numbers during the years 1826 and 1848 were reconstructed by Wolf (1859) himself from the original diaries of Schwabe, and from the values provided for the years 1849 to 1867 it is not known if they were calculated by the same principles. Thus, this scale transfer has to be analyzed further.

## 6 Conclusions

In the archives of the former Swiss Federal Observatory, a manuscript was found containing the raw data of the entire Wolf series from 1610 to 1876 (Wolf 1878a). Now, the Wolf numbers as provided by WDC-SILSO version 1.0 can be reconstructed in every detail, since the source book contains all the raw sunspot group and individual spot numbers as well as the implemented calibration and interpolation methods. In this article we digitized and published the hitherto unknown daily numbers of sunspot groups and individual spots Rudolf Wolf observed from 1849 to 1893 with his three main instruments on the site www.wolfinstitute.ch . Thus, a thorough homogeneity testing of the Wolfian period, acting in fact as the core part of the Wolf series, has become possible, including the widely disregarded scale transfer from the 83/1320 mm Fraunhofer refractor – the standard instrument of the Wolf series – to the 40/700 mm Parisian refractor. Furthermore, a detailed reanalysis and correction of the effects of Wolf’s eyesight diminishment on the homogeneity of the Wolf series can now be done.

## Notes

### Acknowledgements

The author thanks Markus Schenker for the design and implementation of the digitalized source book at www.wolfinstitute.ch .

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