Simulation of the generation of the toroidal magnetic field of the Sun by differential rotation
Heading:
| 1Loginov, AA, 2Krivodubskij, VN, 1Salnikov, NN, 1Prutsko, YV 1Space Research Institute under NAS and National Space Agency of Ukraine, Kyiv, Ukraine 2Astronomical Observatory of Taras Shevchenko National University of Kyiv, Kyiv, Ukraine |
| Kinemat. fiz. nebesnyh tel (Online) 2017, 33(6):17-33 |
| https://doi.org/10.15407/kfnt2017.06.017 |
| Start Page: Solar Physics |
| Language: Russian |
Abstract: Within the framework of the kinematic dynamo theory, we constructed a mathematical model for the evolution of the toroidal magnetic field of the Sun, excited by the differential rotation of the convective zone in the presence of the poloidal field of relic origin. We used the velocity profile obtained as a result of decoding the data of helioseismological experiments. For the model of ideal magnetic hydrodynamics, we calculated the latitudinal profiles of a toroidal field that increases in time for different depths in the solar convection zone. It is found that in the region of differential rotation, the exciting toroidal field is characterized by substantial fluctuations in its magnitude depend on the depth. On the basis of our simulations results, we proposed an explanation for the «incorrect polarity» of magnetic bipolar groups of spots in solar cycles. |
| Keywords: helioseismology, the Sun, toroidal magnetic field |
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