Variation of Stellar Envelope Convection and Overshoot with Metallicity

Abstract

We examine how metallicity affects convection and overshoot in the superadiabatic layer of main sequence stars. We present results from a grid of 3D radiation hydrodynamic simulations with four metallicities ($Z=0.040$, 0.020, 0.010, 0.001), and spanning a range in effective temperature ($4950<{\mathrm{T}}_{\mathrm{eff}}<6230$). We show that changing the metallicity alters properties of the convective gas dynamics, and the structure of the superadiabatic layer and atmosphere. Our grid of simulations show that the amount of superadiabaticity, which tracks the transition from efficient to inefficient convection, \rev{is sensitive to changes in metallicity. We find that increasing the metallicity forces the location of the transition region to lower densities and pressures, and results in larger mean and turbulent velocities throughout the superadiabatic region.} We also quantify the degree of convective overshoot in the atmosphere, and show that it increases with metallicity as well.

Accepted for publication in ApJ

References in corpus (2)

• 3D Hydrodynamical Simulations of Surface Convection in Red Giant Stars. Impact on spectral line formation and abundance analysis
• 3D hydrodynamical CO5BOLD model atmospheres of red giant stars: I. Atmospheric structure of a giant located near the RGB tip

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