Abstract
Abstract We have combined the thermo-chemical disc code ProDiMo with the Monte Carlo radiative transfer code MCFOST to calculate a grid of ∼300 000 circumstellar disc models, systematically varying 11 stellar, disc and dust parameters including the total disc mass, several disc shape parameters and the dust-to-gas ratio. For each model, dust continuum and line radiative transfer calculations are carried out for 29 far-infrared, sub-mm and mm lines of [Oi], [Cii], 12CO and o/p-H2O under five inclinations. The grid allows us to study the influence of the input parameters on the observables, to make statistical predictions for different types of circumstellar discs and to find systematic trends and correlations between the parameters, the continuum fluxes and the line fluxes. The model grid, comprising the calculated disc temperature and chemical structures, the computed spectral energy distributions, line fluxes and profiles, will be used in particular for the data interpretation of the HERSCHEL open time-key program GASPS. The calculated line fluxes show a strong dependence on the assumed ultraviolet excess of the central star and on the disc flaring. The fraction of models predicting [Oi] and [Cii] fine-structure lines fluxes above HERSCHEL/PACS and SPICA/SAFARI detection limits is calculated as a function of disc mass. The possibility of deriving the disc gas mass from line observations is discussed.
Highlights
The structure, composition and evolution of protoplanetary discs are important corner stones to unravel the mystery of life, as they set the initial conditions for planet formation
We note that an unmindful usage of equation (A3) with an assumed value for Texc (e.g. 27 K) for the purpose of gas mass determination from a measured [O I] 63.2 μm line flux can be misleading and does not account for the variety of results that we find in the DENT model grid
In a concerted effort of the theory groups in Edinburgh, Grenoble and Groningen, we have computed a grid of 300 000 circumstellar disc models, simultaneously solving gas-phase, UV-photo and ice
Summary
The structure, composition and evolution of protoplanetary discs are important corner stones to unravel the mystery of life, as they set the initial conditions for planet formation. The DENT grid is a tool to investigate the influence of stellar, disc and dust properties (Table 1) on continuum and line observations (Table 2) and to study in how far these dependences can be inverted.
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