Cooling and Heating of Gas¶
Enzo features a number of different methods for including radiative
cooling. These range from simple tabulated, analytical approximations
to very sophisticated non-equilibrium primoridal chemistry. All of
these methods require the parameter
RadiativeCooling be set to 1.
Other parameters are required for using the various methods, which are
For relevant parameters, please also see Cooling Parameters.
MultiSpecies = 0: Sarazin & White¶
Source: solve_cool.F, cool1d.F
RadiativeCooling = 1
MultiSpecies = 0
This method uses an analytical approximation from Sarazin & White (1987, ApJ, 320, 32) for a fully ionized gas with metallicity of 0.5 solar. This cooling curve is valid over the temperature range from 10,000 K to 109 K. Since this assumes a fully ionized gas, the cooling rate is effectively zero below 10,000 K.
Note: In order use this cooling method, you must copy the file, cool_rates.in, from the input directory into your simulation directory.
MultiSpecies = 1, 2, or 3: Primordial Chemistry and Cooling¶
Source: multi_cool.F, cool1d_multi.F
This method follows the nonequilibrium evolution of primordial
(metal-free) gas. The chemical rate equations are solved using a
semi-implicit backward differencing scheme described by Abel et
al. (1997, New Astronomy, 181) and Anninos et al. (1997, New
Astronomy, 209). Heating and cooling processes include atomic line
excitation, recombination, collisional excitation, free-free
transitions, Compton scattering of the cosmic microwave background and
photoionization from a variety of metagalactic UV backgrounds. For
MultiSpecies > 1, molecular cooling is also included and UV
backgrounds that include photodissociation may also be used.
Numerous chemistry and cooling rates have been added or updated. For
the exact reference for any given rate, users are encouraged to
Only atomic species, H, H+, He, He+, He++, and e- are followed. Since molecular species are not treated, the cooling is effectively zero for temperatures below roughly 10,000 K.
Along with the six species above, H2, H2+, and H- are also followed. In addition to the rates described in Abel et al. (1997) and Anninos et al. (1997), H2 formation via three-body reactions as described by Abel, Bryan, and Norman (2002, Science, 295, 93) is also included. This method is valid in the temperature range of 1 K to 108 K and up to number densities of roughly 109 cm-3. Additionally, three-body heating (4.48eV per molecule formed or dissociated) is added as appropriate.
In addition to the nine species solved with
MultiSpecies= 2, D, D+, and HD are also followed. The range of validity is the same as for
Three distinct methods to calculate the cooling from elements heavier
than He exist. These are selected by setting the
parameter to 1, 2, or 3.
John Wise’s metal cooling.
Cen et al (1995) cooling. This uses output from a Raymond-Smith code to determine cooling rates from T > 104K. No ionizing background is used in computing cooling rates. This method has not been extensively tested in the context of Enzo.
MultiSpeces= 1, 2, or 3
Cloudy cooling operates in conjunction with the primordial chemistry and cooling from
MultiSpeciesset to 1, 2, or 3. As described in Smith, Sigurdsson, & Abel (2008), Cloudy cooling interpolates over tables of precomputed cooling data using the Cloudy photoionization software (Ferland et al. 1998, PASP, 110, 761, http://nublado.org). The cooling datasets can be from one to five dimensional. The range of validity will depends on the dataset used.
- Density and temperature.
- Density, metallicity, and temperature.
- Density, metallicity, electron fraction, and temperature.
- Density, metallicity, electron fraction, redshift of UV background, and temperature.
See Cloudy Cooling for additional parameters that control the behavior of the Cloudy cooling. For more information on obtaining or creating Cloudy cooling datasets, contact Britton Smith (firstname.lastname@example.org).
UV Meta-galactic Backgrounds¶
A variety of spatially uniform photoionizing and photodissociating
backgrounds are available, mainly by setting the parameter
RadiationFieldType. These radiation backgrounds are redshift
dependent and work by setting the photoionization and photoheating
coeffiecients for H, He, and He+. See
Background Radiation Parameters for the additional parameters that
control the UV backgrounds.