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Convective-core overshoot mixing is a significant uncertainty in stellarevolution. Because numerical simulations and turbulent convection modelspredict exponentially decreasing radial rms turbulent velocity, a populartreatment of the overshoot mixing is to apply a diffusion process withexponentially decreasing diffusion coefficient. It is important to investigatethe parameters of the diffusion coefficient because they determine theefficiency of the mixing in the overshoot region. In this paper, we haveinvestigated the effects of the core overshoot mixing on the properties of thecore in solar models and have constrained the parameters of the overshoot modelby using helioseismic inferences and the observation of the solar 8B neutrinoflux. For solar-mass stars, the core overshoot mixing helps to prolong thelifetime of the convective core developed at the ZAMS. If the strength of themixing is sufficiently high, the convective core in a solar model could survivetill the present solar age, leading to large deviations of the sound-speed anddensity profiles comparing with the helioseismic inferences. The 8B neutrinoflux also favours a radiative solar core. Those provide a constraint on theparameters of the exponential diffusion model of the convective overshootmixing. A limited asteroseismic investigation of 13 Kepler low-mass stars with1.0 < M < 1.5 shows a mass-dependent range of the overshoot parameter. Theovershoot mixing processes for different elements are analyzed in detail. It isfound that the exponential diffusion overshoot model leads to differenteffective overshoot mixing lengths for elements with different nuclearequilibrium timescale.

Core overshoot constrained by the absence of a solar convective core and some solar-like stars