J/A+A/688/A56ivo://CDS.VizieR/J/A+A/688/A56doi:10.26093/cds/vizier.36880056CDSBorrero J.M.Milic I.Pastor Yabar A.Kaithakkal A.J.,de la Cruz Rodriguez J.2024-11-29T20:05:07Z2024-08-01T06:55:02ZCDS support team

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

cds-question@unistra.frthe-sunOne-dimensional, semi-empirical models of the solar atmosphere are widely employed in numerous contexts within solar physics, ranging from the determination of element abundances and atomic parameters to studies of the solar irradiance and from Stokes inversions to coronal extrapolations. These models provide the physical parameters (i.e. temperature, gas pressure, etc.) in the solar atmosphere as a function of the continuum optical depth {tau}c. The transformation to the geometrical z scale (i.e. vertical coordinate) is provided via vertical hydrostatic equilibrium. Our aim is to provide updated, one-dimensional, semi-empirical models of the solar atmosphere as a function of z, but employing the more general case of three-dimensional magneto-hydrostatic equilibrium (MHS) instead of vertical hydrostatic equilibrium (HE). We employed a recently developed Stokes inversion code that, along with non-local thermodynamic equilibrium effects, considers MHS instead of HE. This code is applied to spatially and temporally resolved spectropolarimetric observations of the quiet Sun obtained with the CRISP instrument attached to the Swedish Solar Telescope. We provide average models for granules, intergranules, dark magnetic elements, and overall quiet-Sun as a function of both {tau}c and z from the photosphere to the lower chromosphere. We demonstrate that, in these quiet-Sun models, the effect of considering MHS instead of HE is negligible. However, employing MHS increases the consistency of the inversion results before averaging. We surmise that in regions with stronger magnetic fields (i.e. pores, sunspots, network) the benefits of employing the magneto-hydrostatic approximation will be much more palpable.2024A&A...688A..56Bhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/688/A56CatalogResearchIsServedByTAP VizieR generic servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/688/A56https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/688/A56http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/688/A56https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/688/A56https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/688/A56http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/688/A56GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapdefaultJ/A+A/688/A56/tablea1Average model for the entire quiet SunrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintzVertical directionkmphys.sizeinttaulogarithm of the optical depth at 500nm (in (c)- unit)phys.absorption.opticalDepthfloatTTemperatureKphys.temperaturefloatBzVertical component of the magnetic fieldGphys.magFieldfloatBhHorizontal component of the magnetic fieldGphys.magFieldfloatvzVertical component of the velocitykm/sphys.velocfloatPgGas pressuredyn.cm**-2phys.pressuredoublerho*gGravity forceg.s**-2.cm**-2phys.gravity;arith.diffdoubleLzVertical component of the Lorentz forceg.s**-2.cm**-2phys.angMomentumdoublenelecElectron density in non-LTEcm**-3phys.density;phys.electrondoublenhHydrogen densitycm**-3phys.densitydoubleJ/A+A/688/A56/tablea2Average model only granular regionsrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintzVertical directionkmphys.sizeinttaulogarithm of the optical depth at 500nm (in (c)- unit)phys.absorption.opticalDepthfloatTTemperatureKphys.temperaturefloatBzVertical component of the magnetic fieldGphys.magFieldfloatBhHorizontal component of the magnetic fieldGphys.magFieldfloatvzVertical component of the velocitykm/sphys.velocfloatPgGas pressuredyn.cm**-2phys.pressuredoublerho*gGravity forceg.s**-2.cm**-2phys.gravity;arith.diffdoubleLzVertical component of the Lorentz forceg.s**-2.cm**-2phys.angMomentumdoublenelecElectron density in non-LTEcm**-3phys.density;phys.electrondoublenhHydrogen densitycm**-3phys.densitydoubleJ/A+A/688/A56/tablea3Average model only intergranular regionsrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintzVertical directionkmphys.sizeinttaulogarithm of the optical depth at 500nm (in (c)- unit)phys.absorption.opticalDepthfloatTTemperatureKphys.temperaturefloatBzVertical component of the magnetic fieldGphys.magFieldfloatBhHorizontal component of the magnetic fieldGphys.magFieldfloatvzVertical component of the velocitykm/sphys.velocfloatPgGas pressuredyn.cm**-2phys.pressuredoublerho*gGravity forceg.s**-2.cm**-2phys.gravity;arith.diffdoubleLzVertical component of the Lorentz forceg.s**-2.cm**-2phys.angMomentumdoublenelecElectron density in non-LTEcm**-3phys.density;phys.electrondoublenhHydrogen densitycm**-3phys.densitydoubleJ/A+A/688/A56/tablea4Average model dark magnetic elementTTemperatureKphys.temperaturefloatrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintzVertical directionkmphys.sizeinttaulogarithm of the optical depth at 500nm (in (c)- unit)phys.absorption.opticalDepthfloatBzVertical component of the magnetic fieldGphys.magFieldfloatBhHorizontal component of the magnetic fieldGphys.magFieldfloatvzVertical component of the velocitykm/sphys.velocfloatPgGas pressuredyn.cm**-2phys.pressuredoublerho*gGravity forceg.s**-2.cm**-2phys.gravity;arith.diffdoubleLzVertical component of the Lorentz forceg.s**-2.cm**-2phys.angMomentumdoublenelecElectron density in non-LTEcm**-3phys.density;phys.electrondoublenhHydrogen densitycm**-3phys.densitydouble