Editing Sunspot number

{{Short description|Measure of sunspot activity}}
{{Misleading|date=August 2022}}
[[Image:Zurich sunspot number since 1750.png|thumb|350px|Wolf number since 1750.]]

The '''Wolf number''' (also known as the '''relative sunspot number''' or '''Zürich number''') is a quantity that measures the number of [[sunspots]] and groups of sunspots present on the surface of the Sun. Historically, it was only possible to detect [[Sunspot|sunspots]] on the far side of the Sun indirectly using [[helioseismology]]. Since 2006, NASA's [[STEREO]] spacecrafts allow their direct observation.

== History ==
Astronomers have been observing the Sun recording information about sunspots since the advent of the telescope in 1609.<ref>{{cite book|first1 = Jose M.|last1 = Vaquero|first2 = M.|last2 = Vazquez|title=The Sun Recorded Through History|publisher=Springer New York|year=2009|isbn=978-0-387-92790-9|doi = 10.1007/978-0-387-92790-9}}</ref>
However, the idea of compiling the information about the sunspot number from various observers originates in [[Rudolf Wolf]] in 1848<ref>{{cite web|title=The Sun - History|url=http://www-istp.gsfc.nasa.gov/Education/whsun.html|date=2001-11-25|access-date=2012-01-08}}</ref> in [[Zürich]], [[Switzerland]]. The produced series initially had his name, but now it is more commonly referred to as the international sunspot number series.

The international sunspot number series is still being produced today at the observatory of Brussels.<ref>[http://sidc.oma.be/ SIDC], RWC Belgium, World Data Center for the Sunspot Index, [[Observatoire Royal de Belgique|Royal Observatory of Belgium]], 'year(s)-of-data'.</ref> The international number series shows an approximate periodicity of 11 years, the [[solar cycle]], which was first found by [[Heinrich Schwabe]] in 1843, thus sometimes it is also referred to as the Schwabe cycle. The periodicity is not constant but varies roughly in the range 9.5 to 11 years.<ref>Using data from [http://sidc.oma.be/index.php3 SIDC] for the last 300 years and running a fast [[Discrete Fourier transform|FFT]] function on the data gives an average maximum at 10.4883 years/cycle.</ref> The international sunspot number series extends back to 1700 with annual values while daily values exist only since 1818.

Since 1 July 2015 a revised and updated international sunspot number series has been made available.<ref>[http://www.stce.be/press/01/welcome.html Switching to the new Sunspot Number (1 July 2015)]</ref>  The biggest difference is an overall increase by a factor of 1.6 to the entire series.  Traditionally, a scaling of 0.6 was applied to all sunspot counts after 1893, to compensate for Alfred Wolfer's better equipment, after taking over from Wolf.  This scaling has been dropped from the revised series, making modern counts closer to their raw values.  Also, counts were reduced slightly after 1947 to compensate for bias introduced by a new counting method adopted that year, in which sunspots are weighted according to their size.<ref name="clette14" />

==Calculation==
The relative sunspot number <math>R</math> is computed using the formula
: <math>R = k(10g + s) </math>
where
* <math>s</math> is the number of individual spots,
* <math>g</math> is the number of sunspot groups, and
* <math>k</math> is a factor that varies with observer and is referred to as the ''observatory factor'' or the ''personal reduction coefficient''.
The observatory factor compensates for the differing number of recorded individual sunspots and sunspot groups by different observers. These differences in recorded values occur due to differences in instrumentation, local seeing, personal experience, and other factors between observers. Since Wolf was the primary observer for the relative sunspot number, his observatory factor was 1.<ref name="clette14">{{cite journal |last1=Clette |first1=Frédéric |last2=Svalgaard |first2=Leif |last3=Vaquero |first3=José M. |last4=Cliver |first4=Edward W. |title=Revisiting the Sunspot Number: A 400-Year Perspective on the Solar Cycle |journal=Space Science Reviews |date=December 2014 |volume=186 |issue=1–4 |pages=35–103 |doi=10.1007/s11214-014-0074-2|arxiv=1407.3231 |bibcode=2014SSRv..186...35C |s2cid=118511982 }}</ref><ref name="clette07">{{cite journal |last1=Clette |first1=Frédéric |last2=Berghmans |first2=David |last3=Vanlommel |first3=Petra |last4=Van der Linden |first4=Ronald A.M. |last5=Koeckelenbergh |first5=André |last6=Wauters |first6=Laurence |title=From the Wolf number to the International Sunspot Index: 25 years of SIDC |journal=Advances in Space Research |date=January 2007 |volume=40 |issue=7 |pages=919–928 |doi=10.1016/j.asr.2006.12.045 |bibcode=2007AdSpR..40..919C |url=https://www.sciencedirect.com/science/article/pii/S0273117707001974 |access-date=16 August 2022|url-access=subscription }}</ref>

===Smoothed monthly mean===
To calculate the 13-month smoothed monthly mean sunspot number, which is commonly used to calculate the minima and maxima of solar cycles, a tapered-boxcar smoothing function is used. For a given month <math>m</math>, with a monthly sunspot number of <math>R_m</math>, the smoothed monthly mean <math>R_s</math> can be expressed as
: <math>R_s = (0.5 R_{m-6} + R_{m-5} + \dots+ R_{m-1} + R_{m} + R_{m+1} + \dots + R_{m+5} + 0.5 R_{m+6}) / 12 </math>
where <math>R_{m+n}</math> is the monthly sunspot number <math>n</math> months away from month <math>m</math>. The smoothed monthly mean is intended to dampen any sudden jumps in the monthly sunspot number and remove the effects of the 27-day solar rotation period.<ref>{{cite web |title=What does smoothed monthly mean sunspot number actually mean? {{!}} SILSO |url=https://www.sidc.be/SILSO/faq6 |website=www.sidc.be |access-date=16 August 2022}}</ref>

==Alternative series==
The accuracy of the compilation of the group sunspot number series has been questioned, motivating the development of several alternative series<ref>{{cite journal|last1=Lockwood|display-authors=etal|title=Centennial variations in sunspot number, open solar flux, and streamer belt width: 1. Correction of the sunspot number record since 1874.|journal=J. Geophys. Res. Space Phys.|date=2014|volume=119|issue=7|pages=5172–5182|doi=10.1002/2014JA019970|bibcode=2014JGRA..119.5172L|url=http://centaur.reading.ac.uk/36853/1/308_OSF1_jgra51127.pdf|doi-access=free}}</ref><ref>{{cite journal|last1=Svalgaard|first1=Schatten|title=Reconstruction of the sunspot group number: the backbone method.|journal=Solar Physics|date=2016|volume=291|issue=9–10|page=2653|doi=10.1007/s11207-015-0815-8|arxiv=1506.00755|bibcode=2016SoPh..291.2653S|s2cid=119221326}}</ref><ref>{{cite journal|last1=Usoskin|display-authors=etal|title=A new calibrated sunspot group series since 1749: statistics of active day fractions|journal=Solar Physics|date=2016|volume=291|issue=9–10|pages=2685–2708|doi=10.1007/s11207-015-0838-1|arxiv=1512.06421|bibcode=2016SoPh..291.2685U|s2cid=32791225}}</ref><ref name=":1">{{cite journal|last1=Chatzistergos|first1=T.|display-authors=etal|title=New reconstruction of the sunspot group numbers since 1739 using direct calibration and "backbone" methods|journal=Astron. Astrophys.|date=2017|volume=602|page=A69|doi=10.1051/0004-6361/201630045|arxiv=1702.06183|bibcode=2017A&A...602A..69C|s2cid=55139041}}</ref> suggesting different behavior of sunspot group activity before the 20th century.<ref>{{cite journal|last1=Usoskin|first1=I.|title=A history of solar activity over millennia|journal=Living Reviews in Solar Physics|date=2017|volume=14|issue=1|page=3|doi=10.1007/s41116-017-0006-9|bibcode=2017LRSP...14....3U|arxiv=0810.3972|s2cid=195340740}}</ref>
However, indirect indices of solar activity<ref>{{cite journal|last1=Asvestari|first1=E.|display-authors=etal|title=Assessment of different sunspot number series using the cosmogenic isotope 44Ti in meteorites|journal=Monthly Notices of the Royal Astronomical Society|date=2017|volume=467|issue=2|pages=1608–1613|doi=10.1093/mnras/stx190|doi-access=free |bibcode=2017MNRAS.467.1608A|url=http://centaur.reading.ac.uk/69290/1/2017%20Avestari%20et%20al.%2C%20MNRAS%20stx190.pdf}}</ref><ref>{{cite journal|last1=Wu|first1=C.-J.|display-authors=etal|title=Solar total and spectral irradiance reconstruction over the last 9000 years|journal=Astron. Astrophys.|date=2018|volume=620|page=A120|doi=10.1051/0004-6361/201832956|bibcode=2018A&A...620A.120W|arxiv=1811.03464|s2cid=118843780}}</ref><ref>{{cite journal|last1=Petrovay|first1=K.|title=Solar cycle prediction|journal=Living Reviews in Solar Physics|volume=7|pages=6|date=2019|issue=1 |arxiv=1012.5513|bibcode=2020LRSP...17....2P|doi=10.12942/lrsp-2010-6|doi-access=free |pmid=27194963|pmc=4841181}}</ref> favor the group sunspot number series by Chatzistergos T. et al.<ref name=":1" />

A different index of sunspot activity was introduced in 1998 in the form of the number of groups apparent on the solar disc.<ref>{{cite journal|last1=Hoyt|first1=D.|last2=Schatten|first2=K. H.|title=Group Sunspot Numbers: A New Solar Activity Reconstruction|journal=Solar Physics|date=1998|volume=179|issue=1|pages=189–219|doi=10.1023/A:1005007527816|bibcode=1998SoPh..179..189H|s2cid=189822917}}</ref>
With this index it was made possible to include sunspot data acquired since 1609, being the date of the invention of the telescope.

==See also==
* [[Solar cycle]]
* [[Joy's law (astronomy)]]

==References==
{{reflist}}

==External links==
* [http://cse.ssl.berkeley.edu/segwayed/lessons/sunspots/ The Exploratorium's Guide to Sunspots]
* [http://sidc.oma.be/index.php3 Solar Influences Data Analysis Center (SIDC) for the Sunspot Index]
* [http://solarscience.msfc.nasa.gov/SunspotCycle.shtml NASA Solar Physics Sunspot Cycle page] and [http://solarscience.msfc.nasa.gov/greenwch/spot_num.txt Table of Sunspot Numbers (txt)] by month since 1749 CE

{{The Sun}}

[[Category:Stellar phenomena]]
[[Category:Solar phenomena]]

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