Speaker
Description
We carried out a high-resolution simulation of the solar convection zone and, for the first time, reproduced the solar-like differential rotation without using any manipulation.
The sun rotates differentially with the fast equator and the slow poles, called solar-like differential rotation (DR). The DR is thought to be maintained by the turbulent thermal convection in the convection zone, but recent high-resolution simulations cannot reproduce the solar-like DR, i.e., the fast equator. The small-scale turbulence tends to transport the angular momentum radially inward, and the DR results in the anti-solar-like topology. This problem is one of the most essential mysteries in solar physics, called the convective conundrum. In order to resolve the problem, we carried out an unprecedentedly high-resolution simulation using Fugaku, and the solar-like DR is nicely reproduced. The result shows that the magnetic field is unexpectedly strong and has a dominant role in the angular momentum transport.
