Convection and turbulence are one of important fluid dynamical subjects in astrophysics. For example, the efficiency of energy transport by turbulent convection is an important issue in constructing models of stellar interiors. This is especially true in late type and red giant stars, because outer convective zones extend deeply and energy transport by convection in these regions is important to determine the stellar radii. In cases of accretion disks the efficiency of angular momentum transport by turbulent convection is important in determining disk structures. In general, turbulent convection has strong interactions with rotation and magnetic fields. Hence, in various stages of astrophysical phenomena convection and turbulence are important. Our quantitative understanding of turbulent convection is, however, limited, because turbulence is highly nonlinear phenomena. We present here a few basic topics related to convection.