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Deciphering solar turbulence from sunspots records

Abstract : It is generally believed that sunspots are the emergent part of magnetic flux tubes in the solar interior. These tubes are created at the base of the convection zone and rise to the surface due to their magnetic buoyancy. The motion of plasma in the convection zone being highly turbulent, the surface manifestation of sunspots may retain the signature of this turbulence, including its intermittency. From direct observations of sunspots, and indirect observations of the concentration of cosmogenic isotopes 14C in tree rings or 10Be in polar ice, power spectral densities in frequency are plotted. Two different frequency scalings emerge, depending on whether the Sun is quiescent or active. From direct observations we can also calculate scaling exponents. These testify to a strong intermittency, comparable with that observed in the solar wind.
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Submitted on : Friday, July 9, 2010 - 9:56:54 AM
Last modification on : Wednesday, October 14, 2020 - 4:09:31 AM

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Franck Plunian, G. R. Sarson, R. Stepanov. Deciphering solar turbulence from sunspots records. Monthly Notices of the Royal Astronomical Society, Oxford University Press (OUP): Policy P - Oxford Open Option A, 2009, 400 (1), pp.L47 - L51. ⟨10.1111/j.1745-3933.2009.00760.x⟩. ⟨insu-00499276⟩



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