Solar differential rotation reproduced with high-resolution simulation

TL;DR

This paper demonstrates that high-resolution simulations incorporating small-scale dynamo magnetic fields can successfully reproduce the Sun's observed differential rotation, addressing a longstanding convective conundrum.

Contribution

The study shows that including magnetic fields in high-resolution simulations enables realistic modeling of solar differential rotation without artificial manipulations.

Findings

Successfully reproduced solar-like differential rotation in simulations

Magnetic fields from small-scale dynamo influence thermal convection

Addresses the convective conundrum in solar modeling

Abstract

The Sun rotates differentially with a fast equator and slow pole. Convection in the solar interior is thought to maintain the differential rotation. However, although many numerical simulations have been conducted to reproduce the solar differential rotation, previous high-resolution calculations with solar parameters fall into the anti-solar (fast pole) differential rotation regime. Consequently, we still do not know the true reason why the Sun has a fast-rotating equator. While the construction of the fast equator requires a strong rotational influence on the convection, the previous calculations have not been able to achieve the situation without any manipulations. The problem is called convective conundrum. The convection and the differential rotation in numerical simulations were different from the observations. Here, we show that a high-resolution calculation succeeds in reproducing the solar-like differential rotation. Our calculations indicate that the strong magnetic field generated by a small-scale dynamo has a significant impact on thermal convection. The successful reproduction of the differential rotation, convection, and magnetic field achieved in our calculation is an essential step to understanding the cause of the most basic nature of solar activity, specifically, the 11-year cycle of sunspot activity.