J/A+A/592/A18ivo://CDS.VizieR/J/A+A/592/A18doi:10.26093/cds/vizier.35920018CDSMarchand P.Masson J.Chabrier G.Hennebelle P.Commercon B.Vaytet N.2018-03-13T07:13:57Z2016-07-08T15:47:34ZCDS support team

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

cds-question@unistra.frinterstellar-mediumWe develop a detailed chemical network relevant to calculate the conditions that are characteristic of prestellar core collapse. We solve the system of time-dependent differential equations to calculate the equilibrium abundances of molecules and dust grains, with a size distribution given by size-bins for these latter. These abundances are used to compute the different non-ideal magneto-hydrodynamics resistivities (ambipolar, Ohmic and Hall), needed to carry out simulations of protostellar collapse. For the first time in this context, we take into account the evaporation of the grains, the thermal ionisation of potassium, sodium, and hydrogen at high temperature, and the thermionic emission of grains in the chemical network, and we explore the impact of various cosmic ray ionisation rates. All these processes significantly affect the non-ideal magneto-hydrodynamics resistivities, which will modify the dynamics of the collapse. Ambipolar diffusion and Hall effect dominate at low densities, up to n_H_=10^12^cm-3, after which Ohmic diffusion takes over. We find that the time-scale needed to reach chemical equilibrium is always shorter than the typical dynamical (free fall) one. This allows us to build a large, multi-dimensional multi-species equilibrium abundance table over a large temperature, density and ionisation rate ranges. This table, which we make accessible to the community, is used during first and second prestellar core collapse calculations to compute the non-ideal magneto-hydrodynamics resistivities, yielding a consistent dynamical-chemical description of this process.2016A&A...592A..18Mhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/592/A18CatalogResearchIsServedByTAP VizieR generic servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/592/A18https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/592/A18http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/592/A18https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/592/A18https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/592/A18http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/592/A18GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapdefaultJ/A+A/592/A18/abundTable of chemical abundancesgrains04Abundances of grains0 for bin 4phys.abunddoubleTintIntegration timestime.epochdoublegrains-tTotal abundance of grains-phys.abunddoublegrains02Abundances of grains0 for bin 2phys.abunddoublegrains+3Abundances of grains+ for bin 3phys.abunddoublegrains0tTotal abundance of grains0phys.abunddoublerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintrhoDensitycm**-3phys.densitydoubleTTemperatureKphys.temperaturedoublexiIonisation rates**-1phot.count;em.X-raydoubleeAbundance of electronsphys.abunddoubleMgAbundance of ion metal (Mg, etc.)phys.abunddoubleHCO+Abundance of molecular ion HCO^+^phys.atmol.configurationdoubleH3+Abundance of molecular ion H_3_^+^phys.atmol.configurationdoubleH+Abundance of molecular ion H^+^phys.abunddoubleC+Abundance of molecular ion C^+^phys.atmol.configurationdoubleHe+Abundance of molecular ion He^+^phys.abund.YdoubleK+Abundance of molecular ion K^+^meta.notedoubleNa+Abundance of molecular ion Na^+^phys.atmol.configurationdoublegrains+1Abundances of grains+ for bin 1phys.abunddoublegrains-1Abundances of grains- for bin 1phys.abunddoublegrains01Abundances of grains0 for bin 1phys.abunddoublegrains+2Abundances of grains+ for bin 2phys.abunddoublegrains-2Abundances of grains- for bin 2phys.abunddoublegrains-3Abundances of grains- for bin 3phys.abunddoublegrains03Abundances of grains0 for bin 3phys.abunddoublegrains+4Abundances of grains+ for bin 4phys.abunddoublegrains-4Abundances of grains- for bin 4phys.abunddoublegrains+5Abundances of grains+ for bin 5phys.abunddoublegrains-5Abundances of grains- for bin 5phys.abunddoublegrains05Abundances of grains0 for bin 5phys.abunddoublegrains+tTotal abundance of grains+phys.abunddouble