Disk models¶

Beginners¶

Here we give an introduction on how to run some standard models and how to change some input parameters. We encourage the beginner user to run first a few examples. Various examples can be found in the /examples directory of your ProDiMo installation. One can adapt them to the actual needs.

You should start with the Beginners Guide.

• Code directory structure
• Input and output files
• Setting Parameters
• Standard disk models and examples
• Look at the results

Technical stuff¶

• The spatial grid resolution
• How to exchange files in fits_format
• How to accommodate a large number of reactions (>7000) in a large_network
• How to combine_reaction_rate_lists
• How to switch chemical databases (i.e. KIDA, OSU, UMIST) ChemicalDatabases
• How to run models with different adsorption energies Eads
• How to adapt chemical data files
• How to run a model with time-dependent disk chemistry
• How to rerun a (very) old model
• Control memory consumption
• Custom Lines/Molecules

Star and radiation field¶

• Stellar properties
• Fitting stellar parameters and $E_\mathrm{(B-V)}$ from observations

Disk structure¶

• Parameterized fixed-density structure
• Vertical hydrostatic equilibrium
• Multiple zones
• Rounded inner walls
• Envelope structure
• 1D radial interface
• 2D interface
• Dust settling

Dust properties¶

• Dust opacity parameters
• Position dependent opacities

Continuum Radiative Transfer¶

• Advice for setting parameters for the continuum radiative transfer,
• SED (Spectral Energy Distribution)
• Interstellar (background) radiation fields
• X-ray radiative transfer
• Change the Cosmic Background temperature

Chemistry¶

• $\mathrm{H_2}$ formation model
• X-ray chemistry
• Options for the UV photorates
• UV line and continuum shielding
• Notes on photodesorption
• Automatically generated PAH_chemical_network and grain-surface charge reactions.
• Thermal desorption Transition State Theory
• Grain surface chemistry
• Cosmic Ray (galactic/stellar) ionisation rate
• Grain temperature and size-dependent cosmic-ray induced ice desorption
• Ionization due to radioactive decay
• Detailed PAH heating/cooling and PAH chemistry
• PAH size and abundance
• Activate mixing by eddy-diffusion
• How to automatically create charge exchange and proton exchange reactions
• Set the initial element abundances in 2D
• Location-dependent 13CO/12CO ratio
• Dust charge chemistry

Heating and Cooling¶

• use larger model atoms for O, C, C+, Si+ and H UV and optical pumping.
• run models with mid_IR_lines
• customize CO molecular data for 12CO, 13CO, C18O
• customize the H2O molecular data
• include H as a coolant
• model H2 fluorescence
• customize the OH molecular data
• test IR pumping of the atomic/molecular levels
• use the new escape probability method
• Voigt profile escape probability
• Viscous heating
• Photoelectric heating
• Custom Lines/Molecules

Observables¶

• SED (Spectral Energy Distribution)
• Continuum Images
• Compute visibilities
• Spectral line channel maps