Rotation deeply impacts the structure and the evolution of stars. To build coherent 1D or multi-D stellar construction and evolution models, Wood Ranger Power Shears we must systematically consider the turbulent transport of momentum and matter induced by hydrodynamical instabilities of radial and latitudinal differential rotation in stably stratified thermally diffusive stellar radiation zones. In this work, we examine vertical shear instabilities in these areas. The total Coriolis acceleration with the entire rotation vector at a common latitude is taken into consideration. We formulate the problem by considering a canonical shear stream with a hyperbolic-tangent profile. We perform linear stability evaluation on this base flow using both numerical and asymptotic Wentzel-Kramers-Brillouin-Jeffreys (WKBJ) strategies. Two forms of instabilities are identified and explored: inflectional instability, which happens in the presence of an inflection point in shear move, and inertial instability as a result of an imbalance between the centrifugal acceleration and pressure gradient. Both instabilities are promoted as thermal diffusion turns into stronger or stratification turns into weaker.

Effects of the full Coriolis acceleration are found to be more complex in line with parametric investigations in broad ranges of colatitudes and rotation-to-shear and rotation-to-stratification ratios. Also, new prescriptions for the vertical eddy viscosity are derived to model the turbulent transport triggered by every instability. The rotation of stars deeply modifies their evolution (e.g. Maeder, 2009). Within the case of quickly-rotating stars, such as early-sort stars (e.g. Royer et al., 2007) and younger late-sort stars (e.g. Gallet & Bouvier, 2015), the centrifugal acceleration modifies their hydrostatic structure (e.g. Espinosa Lara & Rieutord, 2013