Utility functions¶

The petitRADTRANS.nat_cst package contains some useful utility functions for generating spectra and observables, the use of which are shown below. It also contains useful constants, see the nat_cst code documentation. First we load the package:

[1]:

import os
from petitRADTRANS import nat_cst as nc


Planck function¶

The planck function $$B_\nu(T)$$, in units of erg/cm$$^2$$/s/Hz/steradian, for a given frequency array, can be generated like this:

[2]:

# Define wavelength array, in cm
lamb = np.logspace(-5,-2,100)
# Convert to frequencies
freq = nc.c / lamb
# Calculate Planck function at 5750 K
planck = nc.b(5750., freq)


Let’s plot the Planck function:

[3]:

# Plot Planck function
import pylab as plt
plt.rcParams['figure.figsize'] = (10, 6)
plt.plot(lamb/1e-4, planck)
plt.xscale('log')
plt.xlabel('Wavelength (micron)')
plt.ylabel('Intensity (erg/cm$^2$/s/Hz/sterad)')
plt.show()
plt.clf()

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PHOENIX and ATLAS9 stellar model spectra¶

Within petitRADTRANS the PHOENIX and ATLAS9 stellar spectra can be used, as described in Appendix A of van Boekel et al. (2012). The PHOENIX model refrence, for stellar effective temperatures < 10,000 K is Husser et al. (2013). The ATLAS9 model references for effective temperatures > 10,000 K are Kurucz (1979, 1992, 1994).

The models can be acessed like this, this is for a 5750 K effective temperature star on the main sequence:

[4]:

stellar_spec = nc.get_PHOENIX_spec(5750)
wlen_in_cm = stellar_spec[:,0]
flux_star = stellar_spec[:,1]


Let’s plot the spectrum, and also overplot the black body flux from the previous section (note the required factor of $$\pi$$ to convert the black body intensity to flux):

[5]:

import pylab as plt
plt.plot(wlen_in_cm/1e-4, flux_star, label = 'PHOENIX model')
plt.plot(lamb/1e-4, np.pi*planck, label = 'black body flux')
plt.title(r'$T_{\rm eff}=5750$ K')
plt.xscale('log')
plt.xlabel('Wavelength (micron)')
plt.ylabel('Surface flux (erg/cm$^2$/s/Hz/sterad)')
plt.legend(loc = 'best', frameon = False)
plt.show()
plt.clf()

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Guillot temperature model¶

In petitRADTRANS, one can use analytical atmospheric P-T profile from Guillot (2010), his Equation 29:

$$T^4 = \frac{3T_{\rm int}^4}{4}\left(\frac{2}{3}+\tau\right) + \frac{3T_{\rm equ}^4}{4}\left[\frac{2}{3}+\frac{1}{\gamma\sqrt{3}}+\left(\frac{\gamma}{\sqrt{3}}-\frac{1}{\gamma\sqrt{3}}\right)e^{-\gamma\tau\sqrt{3}}\right]$$

with $$\tau = P\kappa_{\rm IR}/g$$. Here, $$\tau$$ is the optical depth, $$P$$ the pressure, $$\kappa_{\rm IR}$$ the atmospheric opacity in the IR wavelengths (i.e. the cross-section per unit mass), $$g$$ the atmospheric surface gravity, $$\gamma$$ is the ratio between the optical and IR opacity, $$T_{\rm equ}$$ the atmospheric equilibrium temperature, and $$T_{\rm int}$$ is the planetary internal temperature.

Let’s define an example, all units are cgs units, except for the pressure, which is in bars:

[6]:

kappa_IR = 0.01
gamma = 0.4
T_int = 200.
T_equ = 1500.
gravity = 1e1**2.45

pressures = np.logspace(-6, 2, 100)

temperature = nc.guillot_global(pressures, kappa_IR, gamma, gravity, T_int, T_equ)


Let’s plot the P-T profile:

[7]:

plt.plot(temperature, pressures)
plt.yscale('log')
plt.ylim([1e2, 1e-6])
plt.xlabel('T (K)')
plt.ylabel('P (bar)')
plt.show()
plt.clf()

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