J/A+A/568/A91ivo://CDS.VizieR/J/A+A/568/A91doi:10.26093/cds/vizier.35680091CDSMalygin M.G.Kuiper R.Klahr H.Dullemond C.P.Henning T.2015-02-07T09:15:32Z2014-08-26T11:16:30ZCDS support team

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

cds-question@unistra.frinterstellar-mediumastronomical-modelsIn a molecular cloud dust opacity typically dominates over gas opacity, yet in the vicinities of forming stars dust is depleted, and gas is the sole provider of opacity. In the optically thin circumstellar environments the radiation temperature cannot be assumed to be equal to the gas temperature, hence the two-temperature Planck means are necessary to calculate the radiative equilibrium. By using the two-temperature mean opacity one does obtain the proper equilibrium gas temperature in a circumstellar environment, which is in a chemical equilibrium. A careful consideration of a radiative transfer problem reveals that the equilibrium temperature solution can be degenerate in an optically thin gaseous environment. We compute mean gas opacities based on the publicly available code DFSYNTHE by Kurucz and Castelli. We performed the calculations assuming local thermodynamic equilibrium and an ideal gas equation of state. The values were derived by direct integration of the high-resolution opacity spectrum.2014A&A...568A..91Mhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/568/A91CatalogResearchIsServedByTAP VizieR generic servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/568/A91https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/568/A91http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/568/A91https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/568/A91https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/568/A91http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/568/A91GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapdefaultJ/A+A/568/A91/table1Rosseland and Planck means for 94 temperatures, 126 pressures and 3 metallicitiesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordint[Me/H][-0.3/0.3] Metallicity (-0.3, 0.0, +0.3 ) (G1)log(Sun)phys.abund.FefloatTgas[700/1e06] Gas temperature T_gas_Kphys.temperatureintPgas[1e-09/7.2e+08] Gas pressure P_gas_ (dyn/cm^2^)dPaphys.pressuredoublerhoGas density {rho}g.cm**-3phys.densitydoublekRRosseland mean opacity {kappa}_R_cm**2.g**-1phys.absorption.coeff;stat.meandoublekPPlanck mean opacity {kappa}_P_cm**2.g**-1phys.absorption.coeff;stat.meandoubleJ/A+A/568/A91/table2Two-temperature Planck means for 94 temperatures 126 pressures, 3 metallicities and 10 radiation temperaturesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordint[Me/H][-0.3/0.3] Metallicity (-0.3,0.0,+0.3) (G1)log(Sun)phys.abund.FefloatTrad[3000/50000] Radiation temperature T_rad_Kphys.temperatureintTgas[700/1e+06] Gas temperature T_gas_Kphys.temperatureintPgas[1e-09/7.2e+08] Gas pressure P_gas_ (dyn/cm^2^)dPaphys.pressuredoublerhoGas density {rho}g.cm**-3phys.densitydoublekPTwo-temperature Planck mean opacity {kappa}_P_(T_rad_,T_gas_)cm**2.g**-1phys.absorption.coeff;stat.meandouble