  The Sun's axisymmetric large-scale flows, differential rotation and
meridional circulation, are thought to be maintained by the influence of
rotation on the thermal-convective motions in the solar convection zone. These
large-scale flows are crucial for maintaining the Sun's global magnetic field.
Over the last several decades, our understanding of large-scale motions in the
Sun has significantly improved, both through observational and theoretical
efforts. Helioseismology has constrained the flow topology in the solar
interior, and the growth of supercomputers has enabled simulations that can
self-consistently generate large scale flows in rotating spherical convective
shells. In this chapter, we review our current understanding of solar
convection and the large-scale flows present in the Sun, including those
associated with the recently discovered inertial modes of oscillation. We
discuss some issues still outstanding, and provide an outline of future efforts
needed to address these.
