Generation solar-like differential rotation

Abstract

We analyze the simulation result shown in Hotta & Kusano, 2021 in which the solar-like differential rotation is reproduced. The Sun is rotating differentially with the fast equator and the slow pole. It is widely thought that the thermal convection maintains the differential rotation, but recent high-resolution simulations tend to fail to reproduce the fast equator. This fact is an aspect of one of the biggest problems in solar physics called the convective conundrum. Hotta & Kusano, 2021 succeed in reproducing the solar-like differential rotation without using any manipulation with unprecedentedly high-resolution simulation. In this study, we analyze the simulation data to understand the maintenance mechanism of the fast equator. Our analyses lead to conclusions that are summarized as follows. 1. Superequipatition magnetic field is generated by the compression, which can indirectly convert the massive internal energy to magnetic energy. 2. The efficient small-scale energy transport suppresses large-scale convection energy. 3. Non-Taylor--Proudman differential rotation is maintained by the entropy gradient caused by the anisotropic latitudinal energy transport enhanced by the magnetic field. 4. The fast equator is maintained by the meridional flow mainly caused by the Maxwell stress. The Maxwell stress itself also has a role in the angular momentum transport for fast near-surface equator (we call it the Punching ball effect). The fast equator in the simulation is reproduced not due to the low Rossby number regime but due to the strong magnetic field. This study newly finds the role of the magnetic field in the maintenance of differential rotation.

39 pages, 37 figures, 1 table, published in ApJ

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Cited by in corpus (23)

• Evolution of solar and stellar dynamo theory
• Theory of solar oscillations in the inertial frequency range: Amplitudes of equatorial modes from a nonlinear rotating convection simulation
• Transition from anti-solar to solar-like differential rotation: Dependence on Prandtl number
• The Sun's differential rotation is controlled by high-latitude baroclinically unstable inertial modes
• Solar-like to Antisolar Differential Rotation: A Geometric Interpretation
• Transition of latitudinal differential rotation as a possible cause of weakened magnetic braking of solar-type stars
• Lorentz force mediation of turbulent dynamo transitions
• Low-latitude magnetic flux emergence on rapidly rotating solar-type stars
• Implicit large eddy simulations of global solar convection: effects of numerical resolution in non-rotating and rotating cases
• A Potential New Mechanism for the Butterfly Diagram of the Solar Cycle: Latitude-dependent Radial Flux Transport
• Minimal Roles of Solar Subsurface Meridional Flow in the distributed-shear Babcock-Leighton Dynamo
• Small-scale Dynamo in Cool Stars III. Changes in the photospheres of F3V to M0V stars
• Global Turbulent Solar Convection: a Numerical Path Investigating Key Force Balances in the context of the Convective Conundrum
• Simulations of entropy rain-driven convection
• Investigation of the dependence of angular momentum transport on spatial scales for construction of differential rotation
• Small-scale and large-scale dynamos in global convection simulations of solar-like stars
• Impacts of small-scale dynamo on rotating columnar convection in stellar convection zones
• Magnetic field morphologies in convective zones influenced by a turbulent surface layer
• DISPATCH methods: an approximate, entropy-based Riemann solver for ideal magnetohydrodynamics
• Scale-dependent analysis of angular momentum flux in high-resolution magnetohydrodynamic simulations for solar differential rotation
• Effects of the radiative interior on solar inertial modes
• The Yin-Yang Magnetic Flux Eruption (Yin-Yang-MFE) Code: A Global Corona Magnetohydrodynamic Code with the Yin-Yang grid
• Constraining Global Solar Models through Helioseismic Analysis