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Cycle-dependent and cycle-independent surface tracers of solar magnetic activity

Published online by Cambridge University Press:  03 March 2020

D. D. Sokoloff
Affiliation:
Department of Physics, Moscow State University, 119991, Moscow, Russia email: sokoloff.dd@gmail.com; as.shibalova@physics.msu.ru IZMIRAN, 4 Kaluzhskoe Shosse, Troitsk, Moscow, 142190, Russia email: obridko@izmiran.ru; ilivsh@gmail.com
Obridko
Affiliation:
IZMIRAN, 4 Kaluzhskoe Shosse, Troitsk, Moscow, 142190, Russia email: obridko@izmiran.ru; ilivsh@gmail.com
Livshits
Affiliation:
IZMIRAN, 4 Kaluzhskoe Shosse, Troitsk, Moscow, 142190, Russia email: obridko@izmiran.ru; ilivsh@gmail.com Sternberg State Astronomical Institute, Moscow State University, 119991, Moscow, Russia
A. S. Shibalova
Affiliation:
Department of Physics, Moscow State University, 119991, Moscow, Russia email: sokoloff.dd@gmail.com; as.shibalova@physics.msu.ru
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Abstract

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We consider several tracers of magnetic activity that separate cycle-dependent contributions to the background solar magnetic field from those that are independent of the cycle. The main message is that background fields include two relative separate populations. The background fields with a strength up to 100 Mx cm−2 are very poorly correlated with the sunspot numbers and vary little with the phase of the cycle. In contrast, stronger magnetic fields demonstrate pronounced cyclic behaviour. Small-scale solar magnetic fields demonstrate features of fractal intermittent behaviour, which requires quantification. We investigate how the observational estimate of the solar magnetic flux density B depends on resolution D in order to obtain the scaling In BD = −k In D + a in a reasonably wide range. The quantity k demonstrates cyclic variations typical of a solar activity cycle. k depends on the magnetic flux density, i.e. the ratio of the magnetic flux to the area over which the flux is calculated, at a given instant. The quantity a demonstrates some cyclic variation, but it is much weaker than in the case of k. The scaling is typical of fractal structures. The results obtained trace small-scale action in the solar convective zone and its coexistence with the conventional large-scale solar dynamo based on differential rotation and mirror-asymmetric convection. Here we discuss the message for solar dynamo studies hidden in the above results.

Type
Contributed Papers
Copyright
© International Astronomical Union 2020

References

Obridko, V.N., Livshits, I.M., & Sokoloff, D.D. 2017, MNRAS, 472, 2575 CrossRefGoogle Scholar
Shibalova, A.S., Obridko, V.N., & Sokoloff, D.D. 2017, Solar Phys., 292, 44 CrossRefGoogle Scholar