Hydrodynamic model for generation of global poloidal flow of the Sun

Loginov, A. A.; Salnikov, Nikolay N.; Cheremnykh, O. K.; Krivodubskij, V. N.; Maslova, N. V.

doi:10.15407/knit2011.01.029

Cited by 8 publications

(5 citation statements)

References 7 publications

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“…Our calculations indicated the existence, in the SCZ, of a region in which the latitudinal flow becomes unstable. Further studies showed that this instability is responsible for the generation of all known global hydrodynamic flows on the Sun: constant meridional circulation, zonal changes in the angular velocity (torsional oscillations) [17], and space-time variations of the poloidal circulation [15,16]. Our results are in good agreement with observational data and confirm our assumption that global hydrodynamic flows on the Sun arise due to the instability of differential rotation.…”

Section: Introductionsupporting

confidence: 88%

“…1. A detailed description of the model and research results can be found in works [15][16][17][18][19][20].…”

Section: Yyyyyy Yyyyyy Yyy Yyy Yyymentioning

confidence: 99%

“…Thus, in order to determine all three components of the velocity v, it is necessary to solve the differential equation (15) with variable coefficients relative to the function 𝐴(𝑅, 𝜃, 𝑡). From the structure of Eq.…”

Section: ω Formationmentioning

confidence: 99%

“…The solutions to Eq. ( 15) by the Galerkin method [31] give flows of two types [15]: 1) flows that are symmetric about the equator and 2) flows that are mirrorsymmetric about the equator. In other words, flows whose streamlines do not cross the equator, and flows whose streamlines cross the equator.…”

Section: ω Formationmentioning

confidence: 99%

“…Earlier, we proposed a fairly simple model of the space-time structure of the global flows of the Sun with inductive action [15][16][17][18][19][20]. This model uses data from helioseismological studies on the internal structure of a rotating SCZ.…”

Section: Introductionmentioning

confidence: 99%

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Kinematic Dynamo Model of a Solar Magnetic Cycle

et al. 2023

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The paper deals with the problem of explaining the origin and nature of the space-time variations in the magnetic activity of the Sun. It presents a new hydrodynamic model of the solar magnetic cycle, which uses helioseismological data on the differential rotation of the solar convective zone. The model is based on the hypothesis of the emergence of global flows as a result of the loss of stability of a differentially rotating plasma layer in the convective zone. First, the hydrodynamic global plasma flows are calculated without accounting for the effect of a magnetic field on them. Under this condition, it is shown that the solutions found describe all global flows observed on the surface of the Sun: permanent meridional circulation from the equator to the poles, torsional oscillations and space-time variations of the meridional flow. We conclude that the last two flows are azimuthal and meridional components of a single three-dimensional global hydrodynamic flow. Second, to simulate the dynamics of the magnetic field, the found velocities of global migrating flows and the spatial profile of the angular velocity of the internal differential rotation of the solar convective zone obtained from helioseismic measurements were used. Good coincidences have been obtained between the characteristics of the calculated dynamics of global migrating flows and the variable global magnetic fields generated by them with the observed values on the solar surface. An explanation is given for some phenomena on the surface of the Sun, which could not be explained within the framework of the available models.

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Section: Introductionsupporting

confidence: 88%

“…1. A detailed description of the model and research results can be found in works [15][16][17][18][19][20].…”

Section: Yyyyyy Yyyyyy Yyy Yyy Yyymentioning

confidence: 99%

Section: ω Formationmentioning

confidence: 99%

Section: ω Formationmentioning

confidence: 99%