petitRADTRANS.nat_cst

Module Contents

Functions

b(T, nu)

Returns the Planck function \(B_{\nu}(T)\) in units of

guillot_global(P, kappa_IR, gamma, grav, T_int, T_equ)

Returns a temperature array, in units of K,

get_PHOENIX_spec(temperature)

Returns a matrix where the first column is the wavelength in cm

get_PHOENIX_spec_rad(temperature)

Returns a matrix where the first column is the wavelength in cm

running_mean(x, N)

guillot_global_ret(P, delta, gamma, T_int, T_equ)

guillot_modif(P, delta, gamma, T_int, T_equ, ptrans, alpha)

make_press_temp(rad_trans_params)

make_press_temp_iso(rad_trans_params)

Attributes

c

G

kB

sigma

bar

atm

losch

r_sun

r_jup

r_jup_mean

m_jup

m_sun

AU

pc

amu

nA

R

m_earth

r_earth

L0

molecular_weight

pathinp

spec_path

description

logTempGrid

StarRadGrid

specDats

petitRADTRANS.nat_cst.c = 29979245800.0
petitRADTRANS.nat_cst.G = 6.67384e-08
petitRADTRANS.nat_cst.kB = 1.3806488e-16
petitRADTRANS.nat_cst.sigma = 5.670373e-05
petitRADTRANS.nat_cst.bar = 1000000.0
petitRADTRANS.nat_cst.atm = 1013250.0
petitRADTRANS.nat_cst.losch = 2.68676e+19
petitRADTRANS.nat_cst.r_sun = 69550000000.0
petitRADTRANS.nat_cst.r_jup = 7149200000.0
petitRADTRANS.nat_cst.r_jup_mean = 6991100000.0
petitRADTRANS.nat_cst.m_jup = 1.89813e+30
petitRADTRANS.nat_cst.m_sun = 1.9891e+33
petitRADTRANS.nat_cst.AU = 14959787100000.0
petitRADTRANS.nat_cst.pc = 3.08567758e+18
petitRADTRANS.nat_cst.amu = 1.66053892e-24
petitRADTRANS.nat_cst.nA = 6.0221413e+23
petitRADTRANS.nat_cst.R = 8.3144598
petitRADTRANS.nat_cst.m_earth = 5.9722e+27
petitRADTRANS.nat_cst.r_earth = 637813660.0
petitRADTRANS.nat_cst.L0 = 2.68676e+19
petitRADTRANS.nat_cst.molecular_weight
petitRADTRANS.nat_cst.b(T, nu)

Returns the Planck function \(B_{\nu}(T)\) in units of \(\rm erg/s/cm^2/Hz/steradian\).

Args:
T (float):

Temperature in K.

nu:

numpy array containing the frequency in Hz.

petitRADTRANS.nat_cst.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).

petitRADTRANS.nat_cst.pathinp
petitRADTRANS.nat_cst.spec_path
petitRADTRANS.nat_cst.description
petitRADTRANS.nat_cst.logTempGrid
petitRADTRANS.nat_cst.StarRadGrid
petitRADTRANS.nat_cst.specDats = []
petitRADTRANS.nat_cst.get_PHOENIX_spec(temperature)

Returns a matrix where the first column is the wavelength in cm and the second is the stellar flux \(F_\nu\) in units of \(\rm erg/cm^2/s/Hz\), at the surface of the star. The spectra are PHOENIX models from (Husser et al. 2013), the spectral grid used here was described in van Boekel et al. (2012).

Args:
temperature (float):

stellar effective temperature in K.

petitRADTRANS.nat_cst.get_PHOENIX_spec_rad(temperature)

Returns a matrix where the first column is the wavelength in cm and the second is the stellar flux \(F_\nu\) in units of \(\rm erg/cm^2/s/Hz\), at the surface of the star. The spectra are PHOENIX models from (Husser et al. 2013), the spectral grid used here was described in van Boekel et al. (2012).

UPDATE: It also returns a float that is the corresponding estimate of the stellar radius.

Args:
temperature (float):

stellar effective temperature in K.

petitRADTRANS.nat_cst.running_mean(x, N)
petitRADTRANS.nat_cst.guillot_global_ret(P, delta, gamma, T_int, T_equ)
petitRADTRANS.nat_cst.guillot_modif(P, delta, gamma, T_int, T_equ, ptrans, alpha)
petitRADTRANS.nat_cst.make_press_temp(rad_trans_params)
petitRADTRANS.nat_cst.make_press_temp_iso(rad_trans_params)