Axisymmetric investigation of differential rotation in contracting stellar radiative zones

Context. Stars experience rapid contraction or expansion at different phases of their evolution. Modelling the transport angular momentum and chemical elements occurring during these remains an unsolved problem. Aims. We study a stellar radiative zone undergoing radial investigate induced differential rotation meridional circulation. Methods. consider rotating spherical layer crossed by imposed velocity field that mimics contraction, numerically solve axisymmetric hydrodynamical equations in both Boussinesq anelastic approximations. An extensive parametric is conducted to cover regimes rotation, stable stratification, density stratification are relevant for stars. Results. The circulation result from competition between contraction-driven inward outward dominated either viscosity Eddington–Sweet-type circulation, depending on value P r ( N 0 /Ω ) 2 parameter, where Prandtl number, Brunt–Väisäilä frequency, Ω rate. Taking into account important more realistic fields, also because resulting flow less affected unwanted effects boundary conditions. In weak we derive scaling laws relate amplitude timescale.