Convective overshoot in the interiors of solar-type stars

ORAL

Abstract

Convection is an important phenomena in stars. Within stellar convection zones, the transport of heat, magnetic fields and other quantities is highly non-local. At the boundaries of convection zones, the stratification becomes stable and internal gravity waves dominate the dynamics. The extent to which convection overshoots into stably stratified regions is important for understanding the transport and storage of magnetic fields in solar-like dynamos. Here, using the Dedalus pseudospectral framework, we consider the properties of convective overshoot in simulations of fully-compressible convection at low Mach number in domains that span significant density stratifications. We find that little overshoot occurs under conditions typical for solar-type stars, limiting the role of convective overshoot in governing global-scale solar dynamos.

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Authors

  • Benjamin Brown

    Dept. Astrophysical & Planetary Sciences, University of Colorado -- Boulder, Boulder, CO 80309, USA, Astrophysical and Planetary Sciences, University of Colorado, Boulder, University of Colorado Boulder, University of Colorado

  • Evan Anders

    University of Colorado

  • Keaton Burns

    Dept. Physics, Massachusetts Institute of Technology, Cambridge, MA 02139, USA, Massachusetts Institute of Technology

  • Daniel Lecoanet

    Princeton Center for Theoretical Science, Princeton University, Princeton, NJ 08544, USA, Princeton Center for Theoretical Sciences, Princeton University, Princeton Center for Theoretical Science, Princeton University, Princeton University, Princeton Univ

  • Jeffrey Oishi

    Bates College

  • Geoffrey Vasil

    School of Mathematics & Statistics, University of Sydney, NSW 2006, Australia, School of Mathematics & Statistics, University of Sydney, The University of Sydney, University of Sydney