摘要：Context.Space observations by the CoRoT andKeplermissions have provided a wealth of high-quality seismic data for a large number of stars from the main sequence to the red giant phases. One main goal of these missions is to take advantage of the rich spectra of solar-like oscillations to perform precise determinations of stellar characteristic parameters. To make the best of such data, we need theoretical stellar models with a precise near-surface structure since a near-surface structure of a solar-like star has significant influence on solar-like oscillation frequencies. The mixing-length parameter is a key factor to determine the near-surface structure of stellar models. In current versions of the convection formulations used in stellar evolution codes, the mixing-length parameter is a free parameter that needs to be properly specified.Aims.We aim at determining appropriate values of the mixing-length parameter,α, to be used consistently with the adopted convection formulation when computing stellar evolution models across the Hertzsprung–Russell diagram. This determination is based on 3D hydrodynamical simulation models.Methods.We calibratedαvalues by matching entropy profiles of 1D envelope models with those of hydrodynamical 3D models of solar-like stars produced by the CO5BOLD code. For such calibration, previous works concentrated on the classical mixing-length theory (MLT). We also analyzed full spectrum turbulence (FST) models. To construct the atmosphere in the 1D models, we used the Eddington grayT(τ) relation and that with the solar-calibrated Hopf-like function.Results.For both MLT and FST models with a mixing lengthl = αHp, calibratedαvalues increase with increasing surface gravity or decreasing effective temperature. For the FST models, we carried out an additional calibration using anα*value defined asl = rtop − r + α*Hp, top, whereα*is found to increase with surface gravity and effective temperature. We provide tables of the calibratedαvalues across theTeff–log g plane for solar metallicity. By computing stellar evolution with varyingαbased on our 3Dαcalibration, we find that the change from solarαto varyingαshifts evolutionary tracks particularly for the FST model. As for the correspondence to the 3D models, the solar Hopf-like function generally gives a photospheric-minimum entropy closer to a 3D model than the EddingtonT(τ). The structure below the photosphere depends on the adopted convection model. However, we cannot obtain a definitive conclusion about which convection model gives the best correspondence to the 3D models. This is because each 1D physical quantity is related via an equation of state (EoS), but it is not the case for the averaged 3D quantities. Although the FST models withl = rtop − r + α*Hp, topare found to give the oscillation frequencies closest to the solar observed frequencies, their acoustic cavities are formed with compensatory effects between deviating density and temperature profiles near the top of the convective envelope. In future work, an appropriate treatment of the top part of the 1D convective envelope is necessary, for example, by considering turbulent pressure and overshooting.
