Turbulent Magnetic Field Of Solar Thermal Structure Model

As a non-ideal effect, magnetohydrodynamics is not considered in the stellar structure and evolution. The magnetic fields has the influences on the energy redistribution and the energy transformation. The turbulent magnetic fields which is generated by the turbulence is derived from the magnetohydrodynamics equations. It's form is the contribution of the Reynolds stress tensor and magnetic fluctuating tensor. The main expresses have the three aspects. Firstly, the radial parts of the Reynolds stress tensor and magnetic fluctuating tensor contribute to the pressure, which lead to the changes of the hydrostatic equilibrium equation and some thermodynamics variables. Such as temperature, density, internal energy, adiabatic exponent and adiabatic temperature gradient. In the stellar interior, the Schwardzchild's criterion determines the position of the convective zone. Since the changes the adiabatic temperature gradient and the temperature gradient, we can modify the position of the solar convective zone, especially the bottom of the solar convective zone. So we modified the thermodynamics equilibrium structure of the Sun. Secondly, in the solar convective zone, the non-diagonal parts of the Reynolds stress tensor and magnetic fluctuating tensor cause the angular momentum transport, which correct the boundary condition of the solar structure and evolution. Thirdly, the magnetic energy occupied a part of the total energy at the convective zone, which make the change of the energy flux of the gas. Consequently, the result is that we modify the equation of state, hydrostatic equilibrium equation, the boundary condition and the energy flux. In this paper, we only consider the influence of the radial part of the magnetic fluctuating tensor to the solar equilibrium structure.With the high-quality observation methods increasing, more and more observed data illustrated that there exhibits magnetic activities on the surface of the Sun and the Sun-like star. But the generations of the magnetic activities are not understood clearly. They are expected to be known through the investigation of the physics process of the solar interior.