Commit cc8222cc by Matthieu Schaller

### Changed the name of the temperature delta criterion to an entropy delta...

Changed the name of the temperature delta criterion to an entropy delta criterion in the EAGLE model. Documented the delta and the pressures in the RTD.
parent 3f577a4b
 ... ... @@ -424,14 +424,14 @@ metal-dependent star-formation density threshold following the relation derived by Schaye (2004) _. Above a density threshold :math:n^*_{\rm H}, expressed in number of Hydrogen atoms per (physical) cubic centimeters, the star formation rate is expressed as a pressure-law :math:\dot{m}_* = m_g \times A \times \left( 1 {\rm M_\odot}~{\rm pc^2} \right)^{-n} \times \left(\frac{\gamma}{G_{\rm N}}f_gP\right)^{(n-1)/2}, where :math:n is the exponent of the Kennicutt-Schmidt relation (typically :math:n=1.4) and :math:A is the normalisation of the law (typically :math:A=1.515\times10^{-4} {\rm M_\odot}~{\rm yr^{-1}}~{\rm kpc^{-2}}). :math:m_g is the gas particle mass, :math:\gamma is the adiabatic index, :math:f_g the gas fraction of the disk and :math:P the total pressure of the gas including any subgrid turbulent terms. pressure-law :math:\dot{m}_* = m_g \times A \times \left( 1 {\rm M_\odot}~{\rm pc^2} \right)^{-n} \times \left(\frac{\gamma}{G_{\rm N}}f_gP\right)^{(n-1)/2}, where :math:n is the exponent of the Kennicutt-Schmidt relation (typically :math:n=1.4) and :math:A is the normalisation of the law (typically :math:A=1.515\times10^{-4} {\rm M_\odot}~{\rm yr^{-1}}~{\rm kpc^{-2}} for a Cabrier IMF). :math:m_g is the gas particle mass, :math:\gamma is the adiabatic index, :math:f_g the gas fraction of the disk and :math:P the total pressure of the gas including any subgrid turbulent terms. Once a gas particle has computed its star formation rate, we compute the probability that this particle turns into a star using :math:Prob= ... ... @@ -463,14 +463,15 @@ the figure below. does *not* enter the model at all). The values used to produce this figure are the ones assumed in the reference EAGLE model. In the EAGLE model, the pressure entering the star formation includes pressure from the unresolved turbulence. This is modeled in the form of a polytropic equation of state for the gas :math:P = P_{\rm norm}\left(\frac{\rho}{\rho_0}\right)^{\gamma_{\rm eff}}. For practical reasons, this relation is expressed in term of densities. Note that unlike the entropy floor, this is applied at *all* densities and not only above a certain threshold. This equation of state with the relevant YAML parameters defining it is shown on the figure below. In the Schaye & Dalla Vecchia (2008) _ model, the pressure entering the star formation includes pressure from the unresolved turbulence. This is modeled in the form of a polytropic equation of state for the gas :math:P_{EoS} = P_{\rm norm}\left(\frac{\rho}{\rho_0}\right)^{\gamma_{\rm eff}}. For practical reasons, this relation is expressed in term of densities. Note that unlike the entropy floor, this is applied at *all* densities and not only above a certain threshold. This equation of state with the relevant YAML parameters defining it is shown on the figure below. .. figure:: EAGLE_SF_EOS.svg :width: 400px ... ... @@ -488,17 +489,32 @@ is shown on the figure below. star formation rate. The values used to produce this figure are the ones assumed in the reference EAGLE model. In EAGLE, an entropy floor is already in use, so that the pressure of the gas is mentained high enough to prvent fragmentation of the gas. In such a scenario, there is no need for the internal EoS described above. And, of course, in such a scenario, the gas can have a pressure above the floor. The code hence uses :math:P = \max(P_{\rm gas}, P_{\rm floor}, P_{\rm EoS}). To prevent star formation in non-collapsed objects (for instance at high redshift when the whole Universe has a density above the threshold), we apply an over-density criterion. Only gas with a density larger than a multiple of the critical density for closure can form stars. Finally, to prevent gas much above the entropy floor (that has, for instance, been affected by feedback) from forming stars, an optional entropy margin can be specified. Only gas with an entropy :math:A such that :math:A_{\rm EoS} \leq A < A_{\rm EoS} \times 10^\Delta, with :math:\Delta specified in the parameter file. This defaults to a very large number, essentially removing the limit. In simulations with an entropy floor, the limit is calculated above :math:\max(A_{\rm floor}, A_{EoS}), to be consistent with the pressure used in the star formation law. Additionally to the pressure-law corresponding to the Kennicutt-Schmidt relation described, above, we implement a second density threshold above which the slope of the relationship varies (typically steepens). This is governed by two additional parameters: the density at which the relation changes and the second slope. Finally, we optionally use a maximal density above which any gas particle automatically gets a probability to form a star of 100%. automatically gets a probability to form a star of 100%. The code applying this star formation law is located in the directory src/star_formation/EAGLE/`. To simplify things, all constants are converted ... ... @@ -513,12 +529,12 @@ For a normal EAGLE run, that section of the parameter file reads: EOS_density_norm_H_p_cm3: 0.1 # Physical density used for the normalisation of the EOS assumed for the star-forming gas in Hydrogen atoms per cm^3. EOS_temperature_norm_K: 8000 # Temperature om the polytropic EOS assumed for star-forming gas at the density normalisation in Kelvin. EOS_gamma_effective: 1.3333333 # Slope the of the polytropic EOS assumed for the star-forming gas. KS_normalisation: 1.515e-4 # The normalization of the Kennicutt-Schmidt law in Msun / kpc^2 / yr. KS_exponent: 1.4 # The exponent of the Kennicutt-Schmidt law. min_over_density: 57.7 # The over-density above which star-formation is allowed. KS_normalisation: 1.515e-4 # Normalization of the Kennicutt-Schmidt law in Msun / kpc^2 / yr. KS_exponent: 1.4 # Exponent of the Kennicutt-Schmidt law. min_over_density: 57.7 # Over-density above which star-formation is allowed. KS_high_density_threshold_H_p_cm3: 1e3 # Hydrogen number density above which the Kennicut-Schmidt law changes slope in Hydrogen atoms per cm^3. KS_high_density_exponent: 2.0 # Slope of the Kennicut-Schmidt law above the high-density threshold. EOS_temperature_margin_dex: 0.5 # (Optional) Logarithm base 10 of the maximal temperature difference above the EOS allowed to form stars. EOS_entropy_margin_dex: 0.5 # (Optional) Logarithm base 10 of the maximal entropy above the EOS at which stars can form. KS_max_density_threshold_H_p_cm3: 1e5 # (Optional) Hydrogen number density above which a particle gets automatically turned into a star in Hydrogen atoms per cm^3. threshold_norm_H_p_cm3: 0.1 # Normalisation of the metal-dependant density threshold for star formation in Hydrogen atoms per cm^3. threshold_Z0: 0.002 # Reference metallicity (metal mass fraction) for the metal-dependant threshold for star formation. ... ...
 ... ... @@ -115,7 +115,7 @@ EAGLEStarFormation: min_over_density: 57.7 # The over-density above which star-formation is allowed. KS_high_density_threshold_H_p_cm3: 1e3 # Hydrogen number density above which the Kennicut-Schmidt law changes slope in Hydrogen atoms per cm^3. KS_high_density_exponent: 2.0 # Slope of the Kennicut-Schmidt law above the high-density threshold. EOS_temperature_margin_dex: 0.5 # Logarithm base 10 of the maximal temperature difference above the EOS allowed to form stars. EOS_entropy_margin_dex: 0.5 # Logarithm base 10 of the maximal entropy above the EOS at which stars can form. threshold_norm_H_p_cm3: 0.1 # Normalisation of the metal-dependant density threshold for star formation in Hydrogen atoms per cm^3. threshold_Z0: 0.002 # Reference metallicity (metal mass fraction) for the metal-dependant threshold for star formation. threshold_slope: -0.64 # Slope of the metal-dependant star formation threshold ... ...
 ... ... @@ -116,7 +116,7 @@ EAGLEStarFormation: min_over_density: 57.7 # The over-density above which star-formation is allowed. KS_high_density_threshold_H_p_cm3: 1e3 # Hydrogen number density above which the Kennicut-Schmidt law changes slope in Hydrogen atoms per cm^3. KS_high_density_exponent: 2.0 # Slope of the Kennicut-Schmidt law above the high-density threshold. EOS_temperature_margin_dex: 0.5 # Logarithm base 10 of the maximal temperature difference above the EOS allowed to form stars. EOS_entropy_margin_dex: 0.5 # Logarithm base 10 of the maximal entropy above the EOS at which stars can form. threshold_norm_H_p_cm3: 0.1 # Normalisation of the metal-dependant density threshold for star formation in Hydrogen atoms per cm^3. threshold_Z0: 0.002 # Reference metallicity (metal mass fraction) for the metal-dependant threshold for star formation. threshold_slope: -0.64 # Slope of the metal-dependant star formation threshold ... ...
 ... ... @@ -116,7 +116,7 @@ EAGLEStarFormation: min_over_density: 57.7 # The over-density above which star-formation is allowed. KS_high_density_threshold_H_p_cm3: 1e3 # Hydrogen number density above which the Kennicut-Schmidt law changes slope in Hydrogen atoms per cm^3. KS_high_density_exponent: 2.0 # Slope of the Kennicut-Schmidt law above the high-density threshold. EOS_temperature_margin_dex: 0.5 # Logarithm base 10 of the maximal temperature difference above the EOS allowed to form stars. EOS_entropy_margin_dex: 0.5 # Logarithm base 10 of the maximal entropy above the EOS at which stars can form. threshold_norm_H_p_cm3: 0.1 # Normalisation of the metal-dependant density threshold for star formation in Hydrogen atoms per cm^3. threshold_Z0: 0.002 # Reference metallicity (metal mass fraction) for the metal-dependant threshold for star formation. threshold_slope: -0.64 # Slope of the metal-dependant star formation threshold ... ...
 ... ... @@ -112,7 +112,7 @@ EAGLEStarFormation: min_over_density: 57.7 # The over-density above which star-formation is allowed. KS_high_density_threshold_H_p_cm3: 1e3 # Hydrogen number density above which the Kennicut-Schmidt law changes slope in Hydrogen atoms per cm^3. KS_high_density_exponent: 2.0 # Slope of the Kennicut-Schmidt law above the high-density threshold. EOS_temperature_margin_dex: 0.5 # Logarithm base 10 of the maximal temperature difference above the EOS allowed to form stars. EOS_entropy_margin_dex: 0.5 # Logarithm base 10 of the maximal entropy above the EOS at which stars can form. threshold_norm_H_p_cm3: 0.1 # Normalisation of the metal-dependant density threshold for star formation in Hydrogen atoms per cm^3. threshold_Z0: 0.002 # Reference metallicity (metal mass fraction) for the metal-dependant threshold for star formation. threshold_slope: -0.64 # Slope of the metal-dependant star formation threshold ... ...
 ... ... @@ -120,7 +120,7 @@ EAGLEStarFormation: min_over_density: 57.7 # The over-density above which star-formation is allowed. KS_high_density_threshold_H_p_cm3: 1e3 # Hydrogen number density above which the Kennicut-Schmidt law changes slope in Hydrogen atoms per cm^3. KS_high_density_exponent: 2.0 # Slope of the Kennicut-Schmidt law above the high-density threshold. EOS_temperature_margin_dex: 0.5 # Logarithm base 10 of the maximal temperature difference above the EOS allowed to form stars. EOS_entropy_margin_dex: 0.5 # Logarithm base 10 of the maximal entropy above the EOS at which stars can form. threshold_norm_H_p_cm3: 0.1 # Normalisation of the metal-dependant density threshold for star formation in Hydrogen atoms per cm^3. threshold_Z0: 0.002 # Reference metallicity (metal mass fraction) for the metal-dependant threshold for star formation. threshold_slope: -0.64 # Slope of the metal-dependant star formation threshold ... ...
 ... ... @@ -111,7 +111,7 @@ EAGLEStarFormation: min_over_density: 57.7 # The over-density above which star-formation is allowed. KS_high_density_threshold_H_p_cm3: 1e3 # Hydrogen number density above which the Kennicut-Schmidt law changes slope in Hydrogen atoms per cm^3. KS_high_density_exponent: 2.0 # Slope of the Kennicut-Schmidt law above the high-density threshold. EOS_temperature_margin_dex: 0.5 # Logarithm base 10 of the maximal temperature difference above the EOS allowed to form stars. EOS_entropy_margin_dex: 0.5 # Logarithm base 10 of the maximal entropy above the EOS at which stars can form. threshold_norm_H_p_cm3: 0.1 # Normalisation of the metal-dependant density threshold for star formation in Hydrogen atoms per cm^3. threshold_Z0: 0.002 # Reference metallicity (metal mass fraction) for the metal-dependant threshold for star formation. threshold_slope: -0.64 # Slope of the metal-dependant star formation threshold ... ...
 ... ... @@ -121,7 +121,7 @@ EAGLEStarFormation: min_over_density: 57.7 # The over-density above which star-formation is allowed. KS_high_density_threshold_H_p_cm3: 1e3 # Hydrogen number density above which the Kennicut-Schmidt law changes slope in Hydrogen atoms per cm^3. KS_high_density_exponent: 2.0 # Slope of the Kennicut-Schmidt law above the high-density threshold. EOS_temperature_margin_dex: 0.5 # Logarithm base 10 of the maximal temperature difference above the EOS allowed to form stars. EOS_entropy_margin_dex: 0.5 # Logarithm base 10 of the maximal entropy above the EOS at which stars can form. threshold_norm_H_p_cm3: 0.1 # Normalisation of the metal-dependant density threshold for star formation in Hydrogen atoms per cm^3. threshold_Z0: 0.002 # Reference metallicity (metal mass fraction) for the metal-dependant threshold for star formation. threshold_slope: -0.64 # Slope of the metal-dependant star formation threshold ... ...
 ... ... @@ -93,10 +93,10 @@ EAGLEStarFormation: gas_fraction: 0.3 # The gas fraction used internally by the model. KS_normalisation: 1.515e-4 # The normalization of the Kennicutt-Schmidt law in Msun / kpc^2 / yr. KS_exponent: 1.4 # The exponent of the Kennicutt-Schmidt law. min_over_density: 57.7 # The over-density above which star-formation is allowed. min_over_density: 57.7 # The over-density above which star-formation is allowed. KS_high_density_threshold_H_p_cm3: 1e3 # Hydrogen number density above which the Kennicut-Schmidt law changes slope in Hydrogen atoms per cm^3. KS_high_density_exponent: 2.0 # Slope of the Kennicut-Schmidt law above the high-density threshold. EOS_temperature_margin_dex: 0.5 # Logarithm base 10 of the maximal temperature difference above the EOS allowed to form stars. EOS_entropy_margin_dex: 0.5 # Logarithm base 10 of the maximal entropy above the EOS at which stars can form. threshold_norm_H_p_cm3: 0.1 # Normalisation of the metal-dependant density threshold for star formation in Hydrogen atoms per cm^3. threshold_Z0: 0.002 # Reference metallicity (metal mass fraction) for the metal-dependant threshold for star formation. threshold_slope: -0.64 # Slope of the metal-dependant star formation threshold ... ...
 ... ... @@ -93,10 +93,10 @@ EAGLEStarFormation: gas_fraction: 0.3 # The gas fraction used internally by the model. KS_normalisation: 1.515e-4 # The normalization of the Kennicutt-Schmidt law in Msun / kpc^2 / yr. KS_exponent: 1.4 # The exponent of the Kennicutt-Schmidt law. min_over_density: 57.7 # The over-density above which star-formation is allowed. min_over_density: 57.7 # The over-density above which star-formation is allowed. KS_high_density_threshold_H_p_cm3: 1e3 # Hydrogen number density above which the Kennicut-Schmidt law changes slope in Hydrogen atoms per cm^3. KS_high_density_exponent: 2.0 # Slope of the Kennicut-Schmidt law above the high-density threshold. EOS_temperature_margin_dex: 0.5 # Logarithm base 10 of the maximal temperature difference above the EOS allowed to form stars. EOS_entropy_margin_dex: 0.5 # Logarithm base 10 of the maximal entropy above the EOS at which stars can form. threshold_norm_H_p_cm3: 0.1 # Normalisation of the metal-dependant density threshold for star formation in Hydrogen atoms per cm^3. threshold_Z0: 0.002 # Reference metallicity (metal mass fraction) for the metal-dependant threshold for star formation. threshold_slope: -0.64 # Slope of the metal-dependant star formation threshold ... ...
 ... ... @@ -369,13 +369,13 @@ EAGLEStarFormation: EOS_temperature_norm_K: 8000 # Temperature om the polytropic EOS assumed for star-forming gas at the density normalisation in Kelvin. EOS_gamma_effective: 1.3333333 # Slope the of the polytropic EOS assumed for the star-forming gas. gas_fraction: 0.25 # (Optional) The gas fraction used internally by the model (Defaults to 1). KS_normalisation: 1.515e-4 # The normalization of the Kennicutt-Schmidt law in Msun / kpc^2 / yr. KS_exponent: 1.4 # The exponent of the Kennicutt-Schmidt law. min_over_density: 57.7 # The over-density above which star-formation is allowed. KS_normalisation: 1.515e-4 # Normalization of the Kennicutt-Schmidt law in Msun / kpc^2 / yr. KS_exponent: 1.4 # Exponent of the Kennicutt-Schmidt law. min_over_density: 57.7 # Over-density above which star-formation is allowed. KS_high_density_threshold_H_p_cm3: 1e3 # Hydrogen number density above which the Kennicut-Schmidt law changes slope in Hydrogen atoms per cm^3. KS_high_density_exponent: 2.0 # Slope of the Kennicut-Schmidt law above the high-density threshold. KS_max_density_threshold_H_p_cm3: 1e5 # (Optional) Density above which a gas particle gets automatically turned into a star in Hydrogen atoms per cm^3 (Defaults to FLT_MAX). EOS_temperature_margin_dex: 0.5 # (Optional) Logarithm base 10 of the maximal temperature difference above the EOS allowed to form stars (Defaults to FLT_MAX). EOS_entropy_margin_dex: 0.5 # (Optional) Logarithm base 10 of the maximal entropy above the EOS at which stars can form. threshold_norm_H_p_cm3: 0.1 # Normalisation of the metal-dependant density threshold for star formation in Hydrogen atoms per cm^3. threshold_Z0: 0.002 # Reference metallicity (metal mass fraction) for the metal-dependant threshold for star formation. threshold_slope: -0.64 # Slope of the metal-dependant star formation threshold ... ...
 ... ... @@ -69,11 +69,11 @@ struct star_formation { /*! Critical overdensity */ double min_over_den; /*! Dalla Vecchia & Schaye temperature criteria */ double temperature_margin_threshold_dex; /*! Dalla Vecchia & Schaye entropy differnce criterion */ double entropy_margin_threshold_dex; /*! 10^Tdex of Dalla Vecchia & SChaye temperature criteria */ double ten_to_temperature_margin_threshold_dex; /*! 10^Tdex of Dalla Vecchia & Schaye entropy difference criterion */ double ten_to_entropy_margin_threshold_dex; /*! gas fraction */ double fgas; ... ... @@ -273,7 +273,7 @@ INLINE static int star_formation_is_star_forming( /* Check the Scahye & Dalla Vecchia 2012 EOS-based temperature critrion */ return (entropy < entropy_eos * starform->ten_to_temperature_margin_threshold_dex); entropy_eos * starform->ten_to_entropy_margin_threshold_dex); } /** ... ... @@ -587,11 +587,11 @@ INLINE static void starformation_init_backend( starform->max_gas_density = starform->max_gas_density_HpCM3 * number_density_from_cgs; starform->temperature_margin_threshold_dex = parser_get_opt_param_double( parameter_file, "EAGLEStarFormation:EOS_temperature_margin_dex", FLT_MAX); starform->entropy_margin_threshold_dex = parser_get_opt_param_double( parameter_file, "EAGLEStarFormation:EOS_entropy_margin_dex", FLT_MAX); starform->ten_to_temperature_margin_threshold_dex = exp10(starform->temperature_margin_threshold_dex); starform->ten_to_entropy_margin_threshold_dex = exp10(starform->entropy_margin_threshold_dex); /* Read the normalization of the metallicity dependent critical * density*/ ... ... @@ -651,7 +651,7 @@ INLINE static void starformation_print_backend( starform->density_threshold_max_HpCM3); message("Temperature threshold is given by Dalla Vecchia and Schaye (2012)"); message("The temperature threshold offset from the EOS is given by: %e dex", starform->temperature_margin_threshold_dex); starform->entropy_margin_threshold_dex); message("Running with a maximum gas density given by: %e #/cm^3", starform->max_gas_density_HpCM3); } ... ...
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