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Turbulent effects of sunspot magnetic field reconstruction

  • Solar Physics
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Abstract

We study the effects of two-dimensional turbulence generated in sunspot umbra due to strong magnetic fields and Alfven oscillations excited in sunspots due to relatively weak magnetic fields on the evolution of sunspots. Two phases of sunspot magnetic field decaying are shown to exist. The initial rapid phase of magnetic field dissipation is due to two-dimensional turbulence. The subsequent slow phase of magnetic field decaying is associated with Alfven oscillations. Our results correspond to observed data that provide evidence for two types of sunspot evolution. The effect of macroscopic diamagnetic expulsion of magnetic field from the convective zone or photosphere toward sunspots is essential in supporting the long-term stability and equilibrium of vertical magnetic flux tubes in sunspots.

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Authors and Affiliations

  1. Astronomical Observatory, Kyiv National Taras Shevchenko University, ul. Observatornaya 3, Kyiv, 04053, Ukraine

    V. N. Krivodubskii

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  1. V. N. Krivodubskii
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Correspondence to V. N. Krivodubskii.

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Original Russian Text © V.N. Krivodubskii, 2012, published in Kinematika i Fizika Nebesnykh Tel, 2012, Vol. 28, No. 5, pp. 37–49.

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Krivodubskii, V.N. Turbulent effects of sunspot magnetic field reconstruction. Kinemat. Phys. Celest. Bodies 28, 232–238 (2012). https://doi.org/10.3103/S0884591312050054

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