Asymptotic Representation of Low-Degree, Higher-Order g +-Modes in Stars Containing a Convective Core

Abstract

AbstractFirst-order asymptotic representations of low-degree, higher-order g +-modes are developed for stars containing a convective core, which is considered to be in isentropic equilibrium. A distinction is made between stars that contain a radiative envelope and stars that contain both an intermediate radiative zone and a convective envelope, besides their convective core. The asymptotic representations are developed on the basis of the fourth-order system of differential equations for the divergence and the radial component of the Lagrangian displacement that is adopted before for the second-order asymptotic representation of low-degree, higher-order p-modes in stars. The asymptotic methods applied are here also two-variable expansions and boundary-layer theory. For the first type of stars, the nodes of the radial component of the Lagrangian displacement are situated in the radiative envelope; for the second type of stars, these nodes are all situated in the intermediate radiative zone apart from one node, which is situated in the convective envelope.KeywordsAsymptotic SolutionRadial ComponentConvective CoreConvective EnvelopeUndetermined FunctionThese keywords were added by machine and not by the authors. This process is experimental and the keywords may be updated as the learning algorithm improves.