Inertial Oscillations and the Rotation Rate Profile of the Sun

Abstract

We have calculated the stream functions of axisymmetric inertial oscillations in a detailed model of the Sun’s convective envelope, using a finite-difference form of the linearized fluid flow equations in a rotating spherical shell. Inertial oscillations are long period oscillations (of the order of one rotation period) for which the Sun’s Coriolis force provides the principal restoring force. The frequencies and low latitude wave numbers of these oscillations are sensitive to both the rotation rate profile and the depth of the convective envelope. We show the effect different rotation rate curves have on the modes by using both frequency versus wave number diagrams and two-dimensional contour plots of the stream functions. We anticipate that if these modes are observed they will provide a useful and needed check of the rotation curves inferred from p-mode oscillations.