A new model for the lower overshoot layer in the Sun

Abstract

We present a model for the lower overshoot layer of the Sun, based on the realistic solar stratification, without the use of a "mixing-length" parameter, by solving the system of Reynolds momentum equations using the closure formalism of Canuto & Dubovikov (1997, 1998). A fixed value of velocity anisotropy is assumed, and the local convection model is assumed to be valid for the convectively unstable layer. In accordance with seismic constraints, overshoot (defined as the amount by which the convectively mixed zone extends beyond its boundary in local theory) is found to be as low as about 6 percent of the pressure scale height, and it is not bounded by a discontinuity from below.

arXiv comment5 pages, 3 figures

References in corpus (4)

• A study of possible temporal and latitudinal variations in the properties of the solar tachocline
• A-star envelopes: a test of local and non-local models of convection
• Turbulent convection: comparing the moment equations to numerical simulations
• The Anisotropy of Low Prandtl Number Turbulent Convection

Cited by in corpus (8)

• A more realistic representation of overshoot at the base of the solar convective envelope as seen by helioseismology
• Solar models with convective overshoot, the solar-wind mass loss, and a PMS disk accretion: helioseismic quantities, Li depletion and neutrino fluxes
• Turbulent convection model in the overshooting region: II. Theoretical analysis
• Spherical-shell boundaries for two-dimensional compressible convection in a star
• Overshooting by convective settling
• A Consistent One-Dimensional Model for the Turbulent Tachocline
• Three-Dimensional Simulations of Massive Stars: II. Age Dependence
• Seismic study of solar convection and overshooting: results of nonlocal convection