  We investigate the dependence of the angular momentum transport (AMT) on the
spatial scales with numerical simulation of solar-like stars. It is thought
that turbulence has an essential role in constructing solar differential
rotation (DR). In a widely used method to analyse the construction mechanism of
DR, the flow is divided into two components, `mean flow' and `turbulence',
where `turbulence' includes a broad spectrum of spatial scales. The features of
the AMT are expected to depend on the scale. In this study, we decompose the
angular momentum flux (AMF) to investigate the dependence of the AMF on the
spatial scale. We compare the results with anti-solar- (fast pole) and
solar-type (fast equator) DR. Our conclusions are summarized as 1. Radially
outward AMT is seen on a large scale (60 Mm < L <120 Mm) in rotationally
constrained systems. 2. Even when the scale-integrated AMF is negative, we
sometimes observe positive AMF on certain scales. 3. Small-scale turbulence
tends to transport the angular momentum radially inward and causes the
anti-solar DR, indicating that high-resolution simulation is a negative factor
for solar-like DR. Our method to decompose the AMF provides a deep
understanding of the angular momentum and construction mechanism of DR.
