Guillot10
Functions
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Returns a temperature array, in units of K, |
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Get a Guillot temperature profile depending on metallicity. |
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Self-luminous retrieval P-T model. |
Module Contents
- Guillot10.guillot_global(P, kappa_IR, gamma, grav, T_int, T_equ)
Returns a temperature array, in units of K, of the same dimensions as the pressure P (in bar). For this the temperature model of Guillot (2010) is used (his Equation 29).
- Args:
- P:
numpy array of floats, containing the input pressure in bars.
- kappa_IR (float):
The infrared opacity in units of \(\\rm cm^2/s\).
- gamma (float):
The ratio between the visual and infrated opacity.
- grav (float):
The planetary surface gravity in units of \(\\rm cm/s^2\).
- T_int (float):
The planetary internal temperature (in units of K).
- T_equ (float):
The planetary equilibrium temperature (in units of K).
- Guillot10.guillot_global_ret(P, delta, gamma, T_int, T_equ)
- Guillot10.guillot_metallic_temperature_profile(pressures, gamma, surface_gravity, intrinsic_temperature, equilibrium_temperature, kappa_ir_z0, metallicity=None)
Get a Guillot temperature profile depending on metallicity.
- Args:
pressures: (bar) pressures of the profile gamma: ratio between visual and infrated opacity surface_gravity: (cm.s-2) surface gravity intrinsic_temperature: (K) intrinsic temperature equilibrium_temperature: (K) equilibrium temperature kappa_ir_z0: (cm2.s-1) infrared opacity metallicity: ratio of heavy elements abundance over H abundance with respect to the solar ratio
- Returns:
temperatures: (K) the temperature at each pressures of the atmosphere
- Guillot10.guillot_modif(P, delta, gamma, T_int, T_equ, ptrans, alpha)
- Guillot10.PT_ret_model(T3, delta, alpha, tint, press, FeH, CO, conv=True)
Self-luminous retrieval P-T model.
- Args:
- T3np.array([t1, t2, t3])
temperature points to be added on top radiative Eddington structure (above tau = 0.1). Use spline interpolation, t1 < t2 < t3 < tconnect as prior.
- deltafloat
proportionality factor in tau = delta * press_cgs**alpha
- alphafloat
power law index in tau = delta * press_cgs**alpha For the tau model: use proximity to kappa_rosseland photosphere as prior.
- tintfloat
internal temperature of the Eddington model
- pressnp.ndarray
input pressure profile in bar
- convbool
enforce convective adiabat yes/no
- COfloat
C/O for the nabla_ad interpolation
- FeHfloat
metallicity for the nabla_ad interpolation
- Returns:
- Tretnp.ndarray
The temperature as a function of atmospheric pressure.