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Solar Physics

, Volume 289, Issue 2, pp 593–602 | Cite as

Cyclic and Long-Term Variation of Sunspot Magnetic Fields

  • Alexei A. PevtsovEmail author
  • Luca Bertello
  • Andrey G. Tlatov
  • Ali Kilcik
  • Yury A. Nagovitsyn
  • Edward W. Cliver
Solar Origins of Space Weather and Space Climate

Abstract

Measurements from the Mount Wilson Observatory (MWO) were used to study the long-term variations of sunspot field strengths from 1920 to 1958. Following a modified approach similar to that presented in Pevtsov et al. (Astrophys. J. Lett. 742, L36, 2011), we selected the sunspot with the strongest measured field strength for each observing week and computed monthly averages of these weekly maximum field strengths. The data show the solar cycle variation of the peak field strengths with an amplitude of about 500 – 700 gauss (G), but no statistically significant long-term trends. Next, we used the sunspot observations from the Royal Greenwich Observatory (RGO) to establish a relationship between the sunspot areas and the sunspot field strengths for cycles 15 – 19. This relationship was used to create a proxy of the peak magnetic field strength based on sunspot areas from the RGO and the USAF/NOAA network for the period from 1874 to early 2012. Over this interval, the magnetic field proxy shows a clear solar cycle variation with an amplitude of 500 – 700 G and a weaker long-term trend. From 1874 to around 1920, the mean value of magnetic field proxy increases by about 300 – 350 G, and, following a broad maximum in 1920 – 1960, it decreases by about 300 G. Using the proxy for the magnetic field strength as the reference, we scaled the MWO field measurements to the measurements of the magnetic fields in Pevtsov et al. (2011) to construct a combined data set of maximum sunspot field strengths extending from 1920 to early 2012. This combined data set shows strong solar cycle variations and no significant long-term trend (the linear fit to the data yields a slope of − 0.2±0.8 G year−1). On the other hand, the peak sunspot field strengths observed at the minimum of the solar cycle show a gradual decline over the last three minima (corresponding to cycles 21 – 23) with a mean downward trend of ≈ 15 G year−1.

Keywords

Magnetic fields Solar cycle Sunspots 

Notes

Acknowledgements

Y.N. and A.T. acknowledge a partial support from the Federal Program “Scientific and Pedagogical Staff of Innovative Russia”, the Russian Foundation for Basic Research (grants Nos. 10-02-00391 and 12-02-00614), and the Programs of the Presidium of Russian Academy of Sciences Nos. 21 and 22. AAP acknowledges funding from NASA’s NNH09AL04I inter agency transfer. National Solar Observatory (NSO) is operated by the Association of Universities for Research in Astronomy, AURA Inc under cooperative agreement with the National Science Foundation (NSF).

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Copyright information

© Springer Science+Business Media Dordrecht 2013

Authors and Affiliations

  • Alexei A. Pevtsov
    • 1
    Email author
  • Luca Bertello
    • 2
  • Andrey G. Tlatov
    • 3
  • Ali Kilcik
    • 4
  • Yury A. Nagovitsyn
    • 5
  • Edward W. Cliver
    • 6
  1. 1.National Solar ObservatorySunspotUSA
  2. 2.National Solar ObservatoryTucsonUSA
  3. 3.Kislovodsk Solar Station of Pulkovo ObservatoryKislovodskRussian Federation
  4. 4.Big Bear Solar ObservatoryBig Bear CityUSA
  5. 5.Pulkovo Astronomical Observatory, Russian Academy of SciencesSt. PetersburgRussian Federation
  6. 6.Space Vehicles DirectorateAir Force Research LaboratorySunspotUSA

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