"""Kelt-9b secondary eclipse example."""
import starry
import matplotlib.pyplot as plt
import numpy as np
import astropy.units as u
# Config
starry.config.lazy = False
# Star
star_map = starry.Map(udeg=2, amp=1)
star_map[1:] = [0.5, 0.25]
star = starry.Primary(star_map,
m=2.50,
mass_unit=u.M_sun,
r=2.36,
length_unit=u.R_sun)
# Planet
kwargs = dict(
m=0.0,
mass_unit=u.earthMass,
porb=1.481,
r=21.1770214,
length_unit=u.earthRad,
inc=87.2,
t0=-0.65625,
)
# Time arrays (secondary eclipse ingress / full phase curve)
t_ingress = np.linspace(0, 0.017, 1000)
def test_reflected_light():
pri = starry.Primary(starry.Map(amp=0), r=1)
sec = starry.Secondary(starry.Map(reflected=True), porb=1.0, r=1)
sys = starry.System(pri, sec)
t = np.concatenate((np.linspace(0.1, 0.4, 50), np.linspace(0.6, 0.9, 50)))
flux = sys.flux(t)
def test_bodies():
pri = starry.Primary(starry.Map())
sec = starry.Secondary(starry.Map(ydeg=1), porb=1.0)
sys = starry.System(pri, sec)
assert sys.primary == pri
assert sys.secondaries[0] == sec
def test_edge_on_eccentric():
# Params
ydeg = 10
u = [0.5, 0.25]
y = 0.1 * np.random.randn((ydeg + 1)**2 - 1)
porb = 1.0
prot = 1.0
amp = 0.25
r = 0.5
m = 0.25
ecc = 0.5
w = 75
t = np.linspace(-0.75, 0.75, 10000)
# Beta version
pri_beta = starry_beta.kepler.Primary(lmax=2)
pri_beta[1], pri_beta[2] = u
sec_beta = starry_beta.kepler.Secondary(lmax=ydeg)
sec_beta[1:, :] = y
sec_beta.porb = porb
sec_beta.prot = prot
sec_beta.L = amp
sec_beta.r = r
sec_beta.a = (G_grav * (1.0 + m) * porb**2 / (4 * np.pi**2))**(1.0 / 3)
sec_beta.inc = 90
sec_beta.Omega = 0
sec_beta.ecc = ecc
sec_beta.w = w
sys_beta = starry_beta.kepler.System(pri_beta, sec_beta)
sys_beta.compute(t)
flux_beta = np.array(sys_beta.lightcurve)
# Compute the time of transit
M0 = 0.5 * np.pi - w * np.pi / 180.0
f = M0
E = np.arctan2(np.sqrt(1 - ecc**2) * np.sin(f), ecc + np.cos(f))
M = E - ecc * np.sin(E)
t0 = (M - M0) * porb / (2 * np.pi)
# Compute the time of eclipse
E = np.arctan2(
np.sqrt(1 - ecc**2) * np.sin(f + np.pi), ecc + np.cos(f + np.pi))
M = E - ecc * np.sin(E)
t_ecl = (M - M0) * porb / (2 * np.pi)
# This is the required phase offset such that the map coefficients
# correspond to what the observer sees at secondary eclipse
theta0 = -(t_ecl - t0) * 360
# Version 1
pri = starry.Primary(starry.Map(udeg=2))
pri.map[1:] = u
sec = starry.Secondary(
starry.Map(ydeg=ydeg, amp=amp),
porb=porb,
r=r,
m=m,
inc=90,
Omega=0,
ecc=ecc,
w=w,
t0=t0,
theta0=theta0,
)
sec.map[1:, :] = y
sys = starry.System(pri, sec)
flux = sys.flux(t)
# Compare
assert np.allclose(flux, flux_beta)
def test_default_system_units():
pri = starry.Primary(starry.Map())
sec = starry.Secondary(starry.Map(), porb=1.0)
sys = starry.System(pri, sec)
assert sys.time_unit == u.day
"""55 cancrie e secondary eclipse example."""
import starry
import matplotlib.pyplot as plt
import numpy as np
import astropy.units as u
# Config
starry.config.lazy = False
# Star
star_map = starry.Map(udeg=2, amp=1)
star_map[1:] = [0.5, 0.25]
star = starry.Primary(star_map,
m=0.905,
mass_unit=u.M_sun,
r=0.943,
length_unit=u.R_sun)
# Planet
kwargs = dict(
m=7.99,
mass_unit=u.earthMass,
porb=0.73654737,
r=1.875,
length_unit=u.earthRad,
inc=83.59,
t0=0.400473685,
)
# Time arrays (secondary eclipse ingress / full phase curve)
t_ingress = np.linspace(0, 0.002, 1000)