In this example, we'll reproduce Figures 1 and 2 in the extinction release paper (Jones et al. 2020).
"Let us begin with a rather extreme case, a synthetic binary comprised of a hot, B-type main sequence star(M=6.5 Msol,Teff=17000 K, and R=4.2 Rsol) anda cool K-type giant (M=1.8 Msol,Teff=4000 K, and R=39.5 Rsol)vin a 1000 day orbit -- a system where, while the temperature difference is large, the luminosities are similar." (Jones et al. 2020)
Let's first make sure we have the latest version of PHOEBE 2.3 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).
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!pip install -I "phoebe>=2.3,<2.4"
As always, let's do imports and initialize a logger and a new bundle. See Building a System for more details.
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import matplotlib
matplotlib.rcParams['text.usetex'] = True
matplotlib.rcParams['pdf.fonttype'] = 42
matplotlib.rcParams['ps.fonttype'] = 42
matplotlib.rcParams['mathtext.fontset'] = 'stix'
matplotlib.rcParams['font.family'] = 'STIXGeneral'
from matplotlib import gridspec
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%matplotlib inline
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import phoebe
from phoebe import u # units
import numpy as np
import matplotlib.pyplot as plt
logger = phoebe.logger('error')
b = phoebe.default_binary()
First we'll define the system parameters
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b.set_value('period', component='binary', value=1000.0*u.d)
b.set_value('teff', component='primary', value=17000*u.K)
b.set_value('teff', component='secondary', value=4000*u.K)
b.set_value('requiv', component='primary', value=4.22173036*u.solRad)
b.set_value('requiv', component='secondary', value=40.732435*u.solRad)
b.flip_constraint('mass@primary', solve_for='sma@binary')
b.set_value('mass', component='primary', value=6.5*u.solMass)
b.flip_constraint('mass@secondary', solve_for='q')
b.set_value('mass', component='secondary', value=1.9145*u.solMass)
And then create three light curve datasets at the same times, but in different passbands
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times = phoebe.linspace(-20, 20, 101)
b.add_dataset('lc', times=times, dataset='B', passband="Johnson:B")
b.add_dataset('lc', times=times, dataset='R', passband="Cousins:R")
b.add_dataset('lc', times=times, dataset='KEP', passband="Kepler:mean")
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Now we'll set some atmosphere and limb-darkening options
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b.set_value_all('atm', 'ck2004')
b.set_value_all('gravb_bol', 0.0)
b.set_value_all('ld_mode_bol', 'manual')
b.set_value_all('ld_func_bol', 'linear')
b.set_value_all('ld_coeffs_bol', [0.0])
And flip the extinction constraint so we can provide E(B-V).
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b.flip_constraint('ebv', solve_for='Av')
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For comparison, we'll run a model without extinction
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b.set_value('ebv', 0.0)
b.run_compute(distortion_method='rotstar', irrad_method='none', model='noext')
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and then another model with extinction
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b.set_value('ebv', 1.0)
b.run_compute(distortion_method='rotstar', irrad_method='none', model='ext')
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Lastly, we'll convert the model fluxes into magnitudes and format the figures.
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Bextmags=-2.5*np.log10(b['value@fluxes@B@ext@model'])
Bnoextmags=-2.5*np.log10(b['value@fluxes@B@noext@model'])
Bextmags_norm=Bextmags-Bextmags.min()+1
Bnoextmags_norm=Bnoextmags-Bnoextmags.min()+1
Bresid=Bextmags_norm-Bnoextmags_norm
Rextmags=-2.5*np.log10(b['value@fluxes@R@ext@model'])
Rnoextmags=-2.5*np.log10(b['value@fluxes@R@noext@model'])
Rextmags_norm=Rextmags-Rextmags.min()+1
Rnoextmags_norm=Rnoextmags-Rnoextmags.min()+1
Rresid=Rextmags_norm-Rnoextmags_norm
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fig=plt.figure(figsize=(12,6))
gs=gridspec.GridSpec(2,2,height_ratios=[4,1],width_ratios=[1,1])
ax=plt.subplot(gs[0,0])
ax.plot(b['value@times@B@noext@model']/1000,Bnoextmags_norm,color='k',linestyle="--")
ax.plot(b['value@times@B@ext@model']/1000,Bextmags_norm,color='k',linestyle="-")
ax.set_ylabel('Magnitude')
ax.set_xticklabels([])
ax.set_xlim([-0.02,0.02])
ax.set_ylim([3.5,0.8])
ax.set_title('(a) Johnson B')
ax2=plt.subplot(gs[0,1])
ax2.plot(b['value@times@R@noext@model']/1000,Rnoextmags_norm,color='k',linestyle="--")
ax2.plot(b['value@times@R@ext@model']/1000,Rextmags_norm,color='k',linestyle="-")
ax2.set_ylabel('Magnitude')
ax2.set_xticklabels([])
ax2.set_xlim([-0.02,0.02])
ax2.set_ylim([3.5,0.8])
ax2.set_title('(b) Cousins Rc')
ax_1=plt.subplot(gs[1,0])
ax_1.plot(b['value@times@B@noext@model']/1000,Bresid,color='k',linestyle='-')
ax_1.set_ylabel(r'$\Delta m$')
ax_1.set_xlabel('Phase')
ax_1.set_xlim([-0.02,0.02])
ax_1.set_ylim([0.05,-0.3])
ax_1.axhline(y=0., linestyle='dashed',color='k',linewidth=0.5)
ax2_1=plt.subplot(gs[1,1])
ax2_1.plot(b['value@times@R@noext@model']/1000,Rresid,color='k',linestyle='-')
ax2_1.set_ylabel(r'$\Delta m$')
ax2_1.set_xlabel('Phase')
ax2_1.set_xlim([-0.02,0.02])
ax2_1.set_ylim([0.05,-0.3])
ax2_1.axhline(y=0., linestyle='dashed',color='k',linewidth=0.5)
plt.tight_layout()
fig.canvas.draw()
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KEPextmags=-2.5*np.log10(b['value@fluxes@KEP@ext@model'])
KEPnoextmags=-2.5*np.log10(b['value@fluxes@KEP@noext@model'])
KEPextmags_norm=KEPextmags-KEPextmags.min()+1
KEPnoextmags_norm=KEPnoextmags-KEPnoextmags.min()+1
KEPresid=KEPextmags_norm-KEPnoextmags_norm
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fig=plt.figure(figsize=(6,6))
gs=gridspec.GridSpec(2,1,height_ratios=[4,1])
ax=plt.subplot(gs[0])
ax.plot(b['value@times@KEP@noext@model']/1000,KEPnoextmags_norm,color='k',linestyle="--")
ax.plot(b['value@times@KEP@ext@model']/1000,KEPextmags_norm,color='k',linestyle="-")
ax.set_ylabel('Magnitude')
ax.set_xticklabels([])
ax.set_xlim([-0.02,0.02])
ax.set_ylim([3.5,0.8])
ax.set_title('Kepler K')
ax_1=plt.subplot(gs[1])
ax_1.plot(b['value@times@KEP@noext@model']/1000,KEPresid,color='k',linestyle='-')
ax_1.set_ylabel(r'$\Delta m$')
ax_1.set_xlabel('Phase')
ax_1.set_xlim([-0.02,0.02])
ax_1.set_ylim([0.05,-0.3])
ax_1.axhline(y=0., linestyle='dashed',color='k',linewidth=0.5)
plt.tight_layout()
fig.canvas.draw()
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