J/A+A/560/A8ivo://CDS.VizieR/J/A+A/560/A8doi:10.26093/cds/vizier.35600008CDSMagic Z.Collet R.Hayek W.Asplund M.2017-07-11T13:08:33Z2013-11-28T08:59:19ZCDS support team

CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France

cds-question@unistra.frastronomical-modelsstellar-atmosphereslate-type-starsWe study the implications of averaging methods with different reference depth scales for 3D hydrodynamical model atmospheres computed with the Stagger-code. The temporally and spatially averaged (hereafter denoted as <3D>) models are explored in the light of local thermodynamic equilibrium (LTE) spectral line formation by comparing spectrum calculations using full 3D atmosphere structures with those from <3D> averages. We explored methods for computing mean <3D> stratifications from the Stagger-grid time-dependent 3D radiative hydrodynamical atmosphere models by considering four different reference depth scales (geometrical depth, column-mass density, and two optical depth scales). Furthermore, we investigated the influence of alternative averages (logarithmic, enforced hydrostatic equilibrium, flux-weighted temperatures). For the line formation we computed curves of growth for FeI and FeII lines in LTE.2013A&A...560A...8Mhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/560/A8CatalogResearchIsServedByTAP VizieR generic servicerelated-toJ/A+A/557/A26 : STAGGER-grid of 3D stellar models. I. (Magic+, 2013)http://www.stagger-stars.net/ : Stagger stars Home Pagehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/560/A8https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/560/A8http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/560/A8https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/560/A8https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/560/A8http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/560/A8GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapdefaultJ/A+A/560/A8/staggerCombined table from original tablesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintTeffi[3935/7053] Effective temperature (input parameter)Kphys.temperaturefloatloggi[1.5/5] Surface gravity (input parameter)log(cm.s**-2)phys.gravityfloat[Fe/H]i[-4/0.5] Metallicity (input parameter)log(Sun)phys.abund.FefloatModelModel namemeta.id;stat.param;meta.modelledcharlogtau[-5/2] log({tau}) ({tau} is the optical depth)phys.absorption.opticalDepthfloatT(o)Temperature at 500nm optical depth {tau}Kphys.temperaturefloatrho(o)Density {rho} at 500nm optical depth {tau}g.cm**-3phys.absorption.opticalDepthdoublePth(o)Thermodynamic pressure [dyne/cm^2^] at {tau}dPaphys.pressuredoublePtb(o)Turbulent pressure [dyne/cm^2^] at {tau}dPaphys.pressuredoublePe(o)Electron pressure [dyne/cm^2^] at {tau}dPaphys.pressuredoubleT(m)Temperature at Mean Rosseland optical depth {tau}, column mass density averagedKphys.temperaturefloatrho(m)Density {rho} at {tau}g.cm**-3phys.densitydoublePth(m)Thermodynamic pressure [dyne/cm^2^] at {tau}dPaphys.pressuredoublePtb(m)Turbulent pressure [dyne/cm^2^] at {tau}dPaphys.pressuredoublePe(m)Electron pressure [dyne/cm^2^] at {tau}dPaphys.pressuredoubleT(R)Temperature at Rosseland optical depth {tau}, Rosseland optical depth averagedKphys.temperaturefloatrho(R)Density {rho} at {tau}g.cm**-3phys.densitydoublePth(R)Thermodynamic pressure [dyne/cm^2^] at {tau}dPaphys.pressuredoublePtb(R)Turbulent pressure [dyne/cm^2^] at {tau}dPaphys.pressuredoublePe(R)Electron pressure [dyne/cm^2^] at {tau}dPaphys.pressuredoubleT(z)Temperature at Mean Rosseland optical depth {tau}, geometrical height averagedKphys.temperaturefloatrho(z)Density {rho} at {tau}g.cm**-3phys.densitydoublePth(z)Thermodynamic pressure [dyne/cm^2^] at {tau}dPasrc.redshiftdoublePtb(z)Turbulent pressure [dyne/cm^2^] at {tau}dPasrc.redshiftdoublePe(z)Electron pressure [dyne/cm^2^] at {tau}dPaphys.pressuredoubleplotSimbad column added by the CDSmeta.ref.urlchar