Comparison of models for dynamical structures of solar plasma
Abstract
Possible mechanisms of generation of dynamical plasma structures are associated with the Schwarzschild criterion for convective instability and with excess energy (heat, magnetic): due to the superadiabatic temperature gradient, the overheated plasma starts to rise. In the framework of Navier-Stokes MHD equations, the complete system of equations for the full axisymmetric plasma model includes equations for the stream function, the azimuthal velocity component, the density change, the flow function of poloidal magnetic field, and the azimuthal component of the magnetic field. Within the framework of ideal hydrodynamics, the simplest plasma model is applicable to the initial stage of generation of plasma structures. In this case, rigorous analytical solutions are constructed from blocks. Within the framework of ideal hydrodynamics, some intermediate model - the refined model considers rotating plasma at the growth stage. In this case, some unidirectional differential rotation occurs. The full model studies the development of structures as rotating plasma from the very beginning to the highest development stage. The velocity field is adjusted to boundary conditions. Velocity components change in a coordinated manner. The stationary axisymmetric ambient magnetic field and its gradients have little effect on the plasma structure and velocity field. The movement structures for all models are similar. Radial flows converge towards the axis at the bottom, and there is an outflow to the periphery near the top of the plasma structure. The maximum vertical velocity component is reached at the center of the axis. Applications of these models to solar structures, including jets, are discussed.
Versions
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BibTeX
@misc{artekha2026comparison,
title = {{Comparison of models for dynamical structures of solar plasma}},
author = {S. N. Artekha},
howpublished = {arXiv},
year = {2026},
month = nov,
doi = {10.48550/arxiv.2611.02818},
eprint = {2611.02818},
archivePrefix = {arXiv},
url = {https://arxiv.org/abs/2611.02818},
note = {CC BY-NC-ND 4.0},
}
RIS
TY - UNPB
TI - Comparison of models for dynamical structures of solar plasma
AU - S. N. Artekha
PY - 2026
DA - 2026/11/02
PB - arXiv
DO - 10.48550/arxiv.2611.02818
UR - https://arxiv.org/abs/2611.02818
AB - Possible mechanisms of generation of dynamical plasma structures are associated with the Schwarzschild criterion for convective instability and with excess energy (heat, magnetic): due to the superadiabatic temperature gradient, the overheated plasma starts to rise. In the framework of Navier-Stokes MHD equations, the complete system of equations for the full axisymmetric plasma model includes equations for the stream function, the azimuthal velocity component, the density change, the flow function of poloidal magnetic field, and the azimuthal component of the magnetic field. Within the framework of ideal hydrodynamics, the simplest plasma model is applicable to the initial stage of generation of plasma structures. In this case, rigorous analytical solutions are constructed from blocks. Within the framework of ideal hydrodynamics, some intermediate model - the refined model considers rotating plasma at the growth stage. In this case, some unidirectional differential rotation occurs. The full model studies the development of structures as rotating plasma from the very beginning to the highest development stage. The velocity field is adjusted to boundary conditions. Velocity components change in a coordinated manner. The stationary axisymmetric ambient magnetic field and its gradients have little effect on the plasma structure and velocity field. The movement structures for all models are similar. Radial flows converge towards the axis at the bottom, and there is an outflow to the periphery near the top of the plasma structure. The maximum vertical velocity component is reached at the center of the axis. Applications of these models to solar structures, including jets, are discussed.
ER -