Simple Cooling Options¶
- RadiativeCooling (external)
This flag (1 - on, 0 - off) controls whether or not a radiative cooling module is called for each grid. There are currently several possibilities, controlled by the value of another flag. See Radiative Cooling and UV Physics Parameters for more information on the various cooling methods. Default: 0
- If the MultiSpecies flag is off, then equilibrium cooling is assumed and one of the following two will happen. If the parameter GadgetCooling is set to 1, the primordial equilibrium code is called (see below). If GadgetCooling is set to 0, a file called cool_rates.in is read to set a cooling curve. This file consists of a set of temperature and the associated cgs cooling rate; a sample compute with a metallicity Z=0.3 Raymond-Smith code is provided in input/cool_rates.in. This has a cutoff at 10000 K (Sarazin & White 1987). Another choice will be input/cool_rates.in_300K which goes further down to 300 K (Rosen & Bregman 1995).
- If the MultiSpecies flag is on, then the cooling rate is computed directly by the species abundances. This routine (which uses a backward differenced multi-step algorithm) is borrowed from the Hercules code written by Peter Anninos and Yu Zhang, featuring rates from Tom Abel. Other varieties of cooling are controlled by the MetalCooling parameter, as discused below.
- RadiativeCoolingModel (external)
- This switches between the tabular look up cooling that is standard (RadiativeCoolingModel=1) and an analytic fit to the Wolfire et al 2003, ApJ, 587, 278 made by Koyama and Inutsuka 2006 (RadiativeCoolingModel = 3, arXiv:astro-ph/0605528). Default: 1
- GadgetCooling (external)
- This flag (1 - on, 0 - off) turns on (when set to 1) a set of routines that calculate cooling rates based on the assumption of a six-species primordial gas (H, He, no H2 or D) in equilibrium, and is valid for temperatures greater than 10,000 K. This requires the file TREECOOL to execute. Default: 0
- GadgetEquilibriumCooling (external)
- An implementation of the ionization equilibrium cooling code used in the GADGET code which includes both radiative cooling and a uniform metagalactic UV background specified by the TREECOOL file (in the amr_mpi/exe directory). When this parameter is turned on, MultiSpecies and RadiationFieldType are forced to 0 and RadiativeCooling is forced to 1. [Not in public release version]
- MetalCooling (external)
- This flag (0 - off, 1 - metal cooling from Glover & Jappsen 2007, 2 - Cen et al (1995), 3 - Cloudy cooling from Smith, Sigurdsson, & Abel 2008) turns on metal cooling for runs that track metallicity. Option 1 is valid for temperatures between 100 K and 108K because it considers fine-structure line emission from carbon, oxygen, and silicon and includes the additional metal cooling rates from Sutherland & Dopita (1993). Option 2 is only valid for temperatures above 104K. Option 3 uses multi-dimensional tables of heating/cooling values created with Cloudy and optionally coupled to the MultiSpecies chemistry/cooling solver. This method is valid from 10 K to 108K. See the Cloudy Cooling parameters below. Default: 0.
- MetalCoolingTable (internal)
- This field contains the metal cooling table required for MetalCooling option 1. In the top level directory input/, there are two files metal_cool.dat and metal_cool_pop3.dat that consider metal cooling for solar abundance and abundances from pair-instability supernovae, respectively. In the same directory, one can find an IDL routine (make_Zcool_table.pro) that generates these tables. Default: metal_cool.dat
- MultiSpecies (external)
- If this flag (1, 2, 3- on, 0 - off) is on, then the code follows not just the total density, but also the ionization states of Hydrogen and Helium. If set to 2, then a nine-species model (including H2, H2+ and H-) will be computed, otherwise only six species are followed (H, H+, He, He+, He++, e-). If set to 3, then a 12 species model is followed, including D, D+ and HD. This routine, like the last one, is based on work done by Abel, Zhang and Anninos. Default: 0
- MultiMetals (external)
- This was added so that the user could turn on or off additional metal fields - currently there is the standard metallicity field (Metal_Density) and two additional metal fields (Z_Field1 and Z_Field2). Acceptable values are 1 or 0, Default: 0 (off).
- ThreeBodyRate (external)
- Which Three Body rate should be used for H2 formation?: 0 = Abel, Bryan, Norman 2002, 1 = PSS83, 2= CW83, 3 = FH07, 4= G08. (Turk et al 2011 covers these)
- CIECooling (external)
- Should CIE (Ripamonti & Abel 2004) cooling be included at high densities?
- H2OpticalDepthApproximation (external)
- Should the H2 cooling be attenuated (RA04)?
- H2FormationOnDust (external)
- Turns on H2 formation on dust grains and gas-grain heat transfer following Omukai (2000). Default: 0 (OFF)
- NumberOfDustTemperatureBins (external)
- Number of dust temperature bins for the dust cooling and H2 formation rates. Default: 250
- DustTemperatureStart (external)
- Minimum dust temperature for dust rates. Default: 1.0
- DustTemperatureEnd (external)
- Maximum dust temperature for dust rates. Default: 1500
- OutputDustTemperature (external)
- Flag to write out the dust temperature field. Default: 0
- PhotoelectricHeating (external)
- If set to be 1, the following parameter will be added uniformly to the gas without any shielding (Tasker & Bryan 2008). Default: 0
- PhotoelectricHeatingRate (external)
- This is the parameter used as Gamma_pe for uniform photoelectric heating. Default: 8.5e-26 erg s^-1 cm^-3
Cloudy cooling from Smith, Sigurdsson, & Abel (2008) interpolates over tables of precomputed cooling data. Cloudy cooling is turned on by setting MetalCooling to 3. RadiativeCooling must also be set to 1. Depending on the cooling data used, it can be coupled with MultiSpecies = 1, 2, or 3 so that the metal-free cooling comes from the MultiSpecies machinery and the Cloudy tables provide only the metal cooling. Datasets range in dimension from 1 to 5. Dim 1: interpolate over temperature. Dim 2: density and temperature. Dim 3: density, metallicity, and temperature. Dim 4: density, metallicity, electron fraction, and temperature. Dim 5: density, metallicity, electron fraction, spectral strength, and temperature. See Smith, Sigurdsson, & Abel (2008) for more information on creating Cloudy datasets.
- CloudyCoolingGridFile (external)
- A string specifying the path to the Cloudy cooling dataset.
- IncludeCloudyHeating (external)
- An integer (0 or 1) specifying whether the heating rates are to be included in the calculation of the cooling. Some Cloudy datasets are made with the intention that only the cooling rates are to be used. Default: 0 (off).
- CMBTemperatureFloor (external)
- An integer (0 or 1) specifying whether a temperature floor is created at the temperature of the cosmic microwave background (TCMB = 2.72 (1 + z) K). This is accomplished in the code by subtracting the cooling rate at TCMB such that Cooling = Cooling(T) - Cooling(TCMB). Default: 1 (on).
- CloudyElectronFractionFactor (external)
- A float value to account for additional electrons contributed by metals. This is only used with Cloudy datasets with dimension greater than or equal to 4. The value of this factor is calculated as the sum of (Ai * i) over all elements i heavier than He, where Ai is the solar number abundance relative to H. For the solar abundance pattern from the latest version of Cloudy, using all metals through Zn, this value is 9.153959e-3. Default: 9.153959e-3.