  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.
