2006/01/30 by T. M. Rogers, Tamara M. Rogers, Gary A. Glatzmaier +1 · 1 citation
Physics and Astronomy · #Gamma-ray bursts and supernovae #Solar and Space Plasma Dynamics #Stellar, planetary, and galactic studies #astro-ph
paper · pdf · doi:10.1086/508482
published as Astrophys.J.653:765-773,2006 · 24 pages, 8 figures, submitted to ApJ
arxiv created 2006/01/30 · openalex publication_date 2006/12/05 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/31
We present numerical simulations of convective overshoot in a two-dimensional model of the solar equatorial plane. The model equations are solved in the anelastic approximation with enhanced thermal conductivity and viscosity for numerical stability. The simulated domain extends from 0.001 to 0.93 R ☉ , spanning both convective and radiative regions. We show that convective penetration leads to a slightly extended, mildly subadiabatic temperature gradient beneath the convection zone, spanning approximately 0.05 H p , below which there is a rapid transition to a strongly subadiabatic region. A slightly higher temperature is maintained in the overshoot region by adiabatic heating from overshooting plumes. This enhanced temperature may partially account for the sound speed discrepancy between the standard solar model and helioseismology. Simulations conducted with tracer particles suggest that a fully mixed region exists down to at least 0.684 R ☉ .