Lambert Scattering (irrad_method='horvat')

Setup

Let's first make sure we have the latest version of PHOEBE 2.0 installed. (You can comment out this line if you don't use pip for your installation or don't want to update to the latest release).



In [ ]:

    
!pip install -I "phoebe>=2.0,<2.1"

As always, let's do imports and initialize a logger and a new bundle. See Building a System for more details.



In [1]:

    
%matplotlib inline



In [2]:

    
import phoebe
from phoebe import u # units
import numpy as np
import matplotlib.pyplot as plt

logger = phoebe.logger('error')

b = phoebe.default_binary()









    



/usr/lib/python2.7/dist-packages/matplotlib/cbook/deprecation.py:106: MatplotlibDeprecationWarning: The mpl_toolkits.axes_grid module was deprecated in version 2.1. Use mpl_toolkits.axes_grid1 and mpl_toolkits.axisartist provies the same functionality instead.
  warnings.warn(message, mplDeprecation, stacklevel=1)

Relevant Parameters

For parameters that affect reflection and heating (irradfrac*) see the tutorial on reflection and heating.

The 'irrad_method' compute option dictates whether irradiation is handled according to the new Horvat scheme which includes Lambert Scattering, Wilson's original reflection scheme, or ignored entirely.



In [3]:

    
print(b['irrad_method'])









    



Parameter: irrad_method@phoebe01@compute
                       Qualifier: irrad_method
                     Description: Which method to use to handle all irradiation effects (reflection, redistribution)
                           Value: wilson
                         Choices: none, wilson, horvat

Influence on Light Curves (fluxes)

Let's (roughtly) reproduce Figure 8 from Prsa et al. 2016 which shows the difference between Wilson and Horvat schemes for various inclinations.

First we'll roughly create a A0-K0 binary and set reasonable albedos.



In [4]:

    
b['teff@primary'] = 11000
b['rpole@primary'] = 2.5
b['gravb_bol@primary'] = 1.0

b['teff@secondary'] = 5000
b['rpole@secondary'] = 0.85

b['q@binary'] = 0.8/3.0

b.flip_constraint('mass@primary', solve_for='sma@binary')
b['mass@primary'] = 3.0



In [5]:

    
print(b.filter(qualifier=['mass', 'rpole', 'teff'], context='component'))









    



ParameterSet: 6 parameters
         rpole@primary@component: 2.5 solRad
          teff@primary@component: 11000.0 K
          mass@primary@component: 3.0 solMass
       rpole@secondary@component: 0.85 solRad
        teff@secondary@component: 5000.0 K
*       mass@secondary@component: 0.799946619822 solMass



In [6]:

    
b['irrad_frac_refl_bol@primary'] = 1.0
b['irrad_frac_refl_bol@secondary'] = 0.6

Now we'll compute the light curves with wilson and horvat irradiation, and plot the relative differences between the two as a function of phase, for several different values of the inclination.

Note that Figure 8 excluded eclipse effects, but that ability is not included in PHOEBE 2.0, so there will be a slight discrepancy for inclinations which exhibit eclipses.



In [7]:

    
phases = np.linspace(0,1,101)
b.add_dataset('lc', times=b.to_time(phases))









    Out[7]:





<ParameterSet: 15 parameters | contexts: compute, dataset>



In [8]:

    
for incl in [0,30,60,90]:
    b.set_value('incl@binary', incl)
    b.run_compute(irrad_method='wilson')
    fluxes_wilson = b.get_value('fluxes', context='model')
    b.run_compute(irrad_method='horvat')
    fluxes_horvat = b.get_value('fluxes', context='model')
    plt.plot(phases, (fluxes_wilson-fluxes_horvat)/fluxes_wilson, label='i={}'.format(incl))
    
plt.xlabel('phase')
plt.ylabel('[F(wilson) - F(horvat)] / F(wilson)')
plt.legend(loc='upper center')
plt.show()