Geophysical fluid dynamics refers to the fluid dynamics of naturally occurring flows, such as oceans and planetary atmospheres on Earth and other planets. These flows are primarily characterized by two elements: stratification and rotation. In this article we investigate the effects of rotation on the dynamics, by neglecting stratification, in a 2D model. We consider the well-known 2D β-plane Navier-Stokes equations in the statistically forced case. Our problem addresses energy-related phenomena associated with the solution of the equations. To maintain the fluid in a turbulent state, we introduce energy into the system through a stochastic force. In the 2D case, a scaling analysis argument indicates a direct cascade of enstrophy and an inverse energy cascade. Following the evolution of the so-called third-order structure function, we compare the behavior of the direct/inverse cascade with the 2D model lacking the Coriolis force, observing that at small scales, the enstrophy flux from larger to smaller scales remains unaffected by the planetary rotation, in contrast to the large scales where the energy flux from smaller to larger scales is dominated by the Coriolis parameter, confirming experimental and numerical observations. In fact, to the best of our knowledge this is the first mathematically rigorous study of the above equations. This is a joint work with Amirali Hannani and Gigliola Staffilani.