Abstract
The main objective of this paper is to investigate the dynamic bifurcation for the granulation convection in the solar photosphere. Based on the dynamic bifurcation theory, which is established by Ma and Wang (Phase transition dynamics, pp. 380-459, 2014), the critical parameters (R,F) condition for the granulation convection is derived. Furthermore, the corresponding R-F-phase diagram is generated. In addition, the bifurcation solution is also obtained with certain assumptions.
Highlights
The atmosphere of the sun is divided into three parts: the bottom layer of the atmosphere is photosphere, the middle layer is chromosphere and the outermost layer is the corona
Inspired by the dynamic theory, which is established by Ma and Wang to study the Rayleigh-Bénard convection and the Taylor problem, we will investigate the dynamic bifurcation for the granulation convection
Section is devoted to getting the RF-phase diagram of granulation under the parametric condition K = and F =, where R is the Rayleigh number, which is related to the difference of temperature T – T, F is a dimensionless parameter, which is related to the magnetic field H, and K is as in ( . ), which is related to the boundary condition H and H
Summary
The atmosphere of the sun is divided into three parts: the bottom layer of the atmosphere is photosphere, the middle layer is chromosphere and the outermost layer is the corona. It worth noting that Kutner analyzed the structure of granulation in his book [ ] He pointed out that the temperature decreases with the increasing height in the photosphere. It is noticed that the granulation convection structure (see Figure ) is similar to the structure of Rayleigh-Bénard convection and the Taylor problem. Inspired by the dynamic theory, which is established by Ma and Wang to study the Rayleigh-Bénard convection and the Taylor problem (see [ , – ]), we will investigate the dynamic bifurcation for the granulation convection. . Section is devoted to getting the RF-phase diagram of granulation under the parametric condition K = and F = , where R is the Rayleigh number, which is related to the difference of temperature T – T , F is a dimensionless parameter, which is related to the magnetic field H, and K is as in
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