Bell_EBM package

Submodules

Bell_EBM.H2_Dissociation_Routines module

Bell_EBM.H2_Dissociation_Routines.cp_H2(T)

Get the isobaric specific heat capacity of H2 as a function of temperature.

Parameters:

T (ndarray) – The temperature.

Returns:

The isobaric specific heat capacity of H2.

Return type:

ndarray

Bell_EBM.H2_Dissociation_Routines.dDissFracApprox(T, mu=3320.680532597579, std=471.38088012739126)

Calculate the derivative in the dissociation fraction of H2 using an erf approximation.

Parameters:

• T (ndarray) – The temperature in K.

• mu (float, optional) – The mean for the Gaussian function.

• std (float, optional) – The standard deviation for the Gaussian function.

Returns:

The derivative in the dissociation fraction of H2.

Return type:

ndarray

Bell_EBM.H2_Dissociation_Routines.dDissFracSaha(T, P)

Calculate the derivative of the dissociation fraction of H2 using the Saha Equation.

Parameters:

• T (ndarray) – The temperature in K.

• P (ndarray) – The pressure in Pa.

Returns:

The derivative of the dissociation fraction of H2.

Return type:

ndarray

Bell_EBM.H2_Dissociation_Routines.delta_cp_H2(T)

Get the derivative of the isobaric specific heat capacity of H2 as a function of temperature.

Pretty sure cp_H2 should already include this factor…

Parameters:

T (ndarray) – The temperature.

Returns:

The derivative of theisobaric specific heat capacity of H2.

Return type:

ndarray

Bell_EBM.H2_Dissociation_Routines.dissFracApprox(T, mu=3320.680532597579, std=471.38088012739126)

Calculate the dissociation fraction of H2 using an erf approximation.

Parameters:

• T (ndarray) – The temperature in K.

• mu (float, optional) – The mean for the error function.

• std (float, optional) – The standard deviation for the error function.

Returns:

The dissociation fraction of H2.

Return type:

ndarray

Bell_EBM.H2_Dissociation_Routines.dissFracSaha(T, P)

Calculate the dissociation fraction of H2 using the Saha Equation.

Parameters:

• T (ndarray) – The temperature in K.

• P (ndarray) – The pressure in Pa.

Returns:

The dissociation fraction of H2.

Return type:

ndarray

Bell_EBM.H2_Dissociation_Routines.getSahaApproxParams(P=10132.5)

Get the Gaussian and erf parameters used to approximate the Saha equation.

Parameters:

P (ndarray) – The pressure in Pa.

Returns:

2 floats containing the mean and the standard deviatio for the Gaussian/erf functions.

Return type:

list

Bell_EBM.H2_Dissociation_Routines.lte_cp(T, mu=3320.680532597579, std=471.38088012739126)

Get the isobaric specific heat capacity of an LTE mix of H2+H as a function of temperature.

Does not account for the energy of H2 dissociation/recombination.

Parameters:

• T (ndarray) – The temperature.

• mu (float) – The mean for the Gaussian/erf approximations to the Saha equation.

• std (float) – The standard deviation for the Gaussian/erf approximations to the Saha equation.

Returns:

The isobaric specific heat capacity of an LTE mix of H2+H.

Return type:

ndarray

Bell_EBM.H2_Dissociation_Routines.nQ(mu, T)

Calculate the quantum concentration.

Parameters:

• mu (ndarray) – The mean molecular weight in units of u.

• T (ndarray) – The temperature in K.

Returns:

The quantum concentration.

Return type:

ndarray

Bell_EBM.H2_Dissociation_Routines.tau_diss(P, T)

Calculate the dissociation timescale.

These are rough estimates based on Shui (1973).

Parameters:

• T (ndarray) – The temperature in K.

• P (ndarray) – The pressure in Pa.

Returns:

The dissociation timescale in s^-1.

Return type:

ndarray

Bell_EBM.H2_Dissociation_Routines.tau_recomb(P, T)

Calculate the recombination timescale.

These are rough estimates based on Shui (1973).

Parameters:

• T (ndarray) – The temperature in K.

• P (ndarray) – The pressure in Pa.

Returns:

The recombination timescale in s^-1.

Return type:

ndarray

Bell_EBM.H2_Dissociation_Routines.true_cp(T, mu=3320.680532597579, std=471.38088012739126)

Get the isobaric specific heat capacity of an LTE mix of H2+H as a function of temperature.

Accounts for the energy of H2 dissociation/recombination.

Parameters:

• T (ndarray) – The temperature.

• mu (float) – The mean for the Gaussian/erf approximations to the Saha equation.

• std (float) – The standard deviation for the Gaussian/erf approximations to the Saha equation.

Returns:

The isobaric specific heat capacity of an LTE mix of H2+H.

Return type:

ndarray

Bell_EBM.KeplerOrbit module

class Bell_EBM.KeplerOrbit.KeplerOrbit(a=149597870700.0, Porb=None, inc=90.0, t0=0.0, e=0.0, Omega=270.0, argp=90.0, obliq=0.0, argobliq=0.0, Prot=None, m1=1.988409870698051e+30, m2=0.0)

Bases: object

A Keplerian orbit.

a

The semi-major axis in m.

Type:

float

inc

The orbial inclination (in degrees above face-on)

Type:

float

t0

The linear ephemeris in days.

Type:

float

e

The orbital eccentricity.

Type:

float

Prot

Body 2’s rotational period in days.

Type:

float

Omega

The longitude of ascending node (in degrees CCW from line-of-sight).

Type:

float

argp

The argument of periastron (in degrees CCW from Omega).

Type:

float

obliq

The obliquity (axial tilt) of body 2 (in degrees toward body 1).

Type:

float, optional

argobliq

The reference orbital angle used for obliq (in degrees from inferior conjunction).

Type:

float, optional

t_peri

Time of body 2’s closest approach to body 1.

Type:

float

t_ecl

Time of body 2’s eclipse by body 1.

Type:

float

mean_motion

The mean motion in radians.

Type:

float

FSSI(Y, x, f, fP)

Fast Switch and Spline Inversion method from Tommasini+2018.

Parameters:

• Y (ndarray) – The f(x) values to invert.

• x (ndarray) – x values spanning the domain (more values for higher precision).

• f (callable) – The function f.

• fP (callable) – The first derivative of the function f with respect to x.

Returns:

The numerical approximation of f^-(y).

Return type:

ndarray

FSSI_Eccentric_Inverse(M, xtol=1e-10)

Convert mean anomaly to eccentric anomaly using FSSI (Tommasini+2018).

Parameters:

• M (ndarray) – The mean anomaly in radians.

• xtol (float) – tolarance on error in eccentric anomaly.

Returns:

The eccentric anomaly in radians.

Return type:

ndarray

Newton_Eccentric_Inverse(M, xtol=1e-10)

Convert mean anomaly to eccentric anomaly using Newton.

Parameters:

• M (ndarray) – The mean anomaly in radians.

• xtol (float) – tolarance on error in eccentric anomaly.

Returns:

The eccentric anomaly in radians.

Return type:

ndarray

property Porb

Body 2’s orbital period in days.

Changing this will update Prot if none was provided when the orbit was initialized.

Type:

float

distance(t=None, TA=None, xtol=1e-10)

Find the separation between the two bodies.

Parameters:

• t (ndarray) – The time in days.

• TA (ndarray) – The true anomaly in radians (if t and TA are given, only TA will be used).

• xtol (float) – tolarance on error in eccentric anomaly (calculated along the way).

Returns:

The separation between the two bodies.

Return type:

ndarray

ea_to_ma(ea)

Convert eccentric anomaly to mean anomaly.

Parameters:

ea (ndarray) – The eccentric anomaly in radians.

Returns:

The mean anomaly in radians.

Return type:

ndarray

eccentric_anomaly(t, useFSSI=None, xtol=1e-10)

Convert time to eccentric anomaly, numerically.

Parameters:

• t (ndarray) – The time in days.

• useFSSI (bool) – Whether or not to use FSSI to invert Kepler’s equation.

• xtol (float) – tolarance on error in eccentric anomaly.

Returns:

The eccentric anomaly in radians.

Return type:

ndarray

get_phase(t, TA=None)

Get the orbital phase.

Parameters:

t (ndarray) – The time in days.

Returns:

The orbital phase.

Return type:

ndarray

get_sop(t)

Calculate the sub-observer longitude and latitude.

Parameters:

t (ndarray) – The time in days.

Returns:

A list of 2 ndarrays containing the sub-observer longitude and latitude.

Each ndarray is in the same shape as t.

Return type:

list

get_ssp(t, TA=None)

Calculate the sub-stellar longitude and latitude.

Parameters:

t (ndarray) – The time in days.

Returns:

A list of 2 ndarrays containing the sub-stellar longitude and latitude.

Each ndarray is in the same shape as t.

Return type:

list

property m1

Body 1’s mass in kg.

If no period was provided when the orbit was initialized, changing this will update the period.

Type:

float

property m2

Body 2’s mass in kg.

If no period was provided when the orbit was initialized, changing this will update the period.

Type:

float

mean_anomaly(t)

Convert time to mean anomaly.

Parameters:

t (ndarray) – The time in days.

Returns:

The mean anomaly in radians.

Return type:

ndarray

property phase_eclipse

The orbital phase of eclipse.

Read-only.

Type:

float

property phase_periastron

The orbital phase of periastron.

Read-only.

Type:

float

property phase_transit

The orbital phase of transit.

Read-only.

Type:

float

plot_orbit()

A convenience routine to visualize the orbit

Returns:

The figure containing the plot.

Return type:

figure

solve_period()

Find the Keplerian orbital period.

Returns:

The Keplerian orbital period.

Return type:

float

property t_trans

Time of body 1’s eclipse by body 2.

Read-only.

Type:

float

ta_to_ea(ta)

Convert true anomaly to eccentric anomaly.

Parameters:

ta (ndarray) – The true anomaly in radians.

Returns:

The eccentric anomaly in radians.

Return type:

ndarray

ta_to_ma(ta)

Convert true anomaly to mean anomaly.

Parameters:

ta (ndarray) – The true anomaly in radians.

Returns:

The mean anomaly in radians.

Return type:

ndarray

true_anomaly(t, xtol=1e-10)

Convert time to true anomaly, numerically.

Parameters:

• t (ndarray) – The time in days.

• xtol (float) – tolarance on error in eccentric anomaly (calculated along the way).

Returns:

The true anomaly in radians.

Return type:

ndarray

xyz(t, xtol=1e-10)

Find the coordinates of body 2 with respect to body 1.

Parameters:

• t (ndarray) – The time in days.

• xtol (float) – tolarance on error in eccentric anomaly (calculated along the way).

Returns:

A list of 3 ndarrays containing the x,y,z coordinate of body 2 with respect to body 1.

The x coordinate is along the line-of-sight. The y coordinate is perpendicular to the line-of-sight and in the orbital plane. The z coordinate is perpendicular to the line-of-sight and above the orbital plane

Return type:

list

Bell_EBM.Map module

class Bell_EBM.Map.Map(values=None, dissValues=None, time=0.0, nlat=16, nlon=None)

Bases: object

A map.

dissValues

The H2 dissociation fraction values for the map.

Type:

ndarray

lat

The unique latitude values in degrees.

Type:

ndarray, optional

lat_radians

The unique latitude values in radians.

Type:

ndarray, optional

latGrid

The latitude grid in degrees.

Type:

ndarray

latGrid_radians

The latitude grid in radians.

Type:

ndarray

lon

The unique longitude values in degrees.

Type:

ndarray, optional

lon_radians

The unique longitude values in radians.

Type:

ndarray, optional

lonGrid

The longitude grid in degrees.

Type:

ndarray

lonGrid_radians

The longitude grid in radians.

Type:

ndarray

nlat

The number of latitudinal cells to use for rectangular maps.

Type:

int, optional

nlon

The number of longitudinal cells to use for rectangular maps.

Type:

int, optional

nside

A parameter that sets the resolution of healpy maps.

Type:

int, optional

pixArea

The area of each pixel.

Type:

ndarray

time

Time of map in days.

Type:

float

useHealpix

Whether the planet’s map uses a healpix grid.

Type:

bool

values

The temperature map values.

Type:

ndarray

plot_H2_dissociation(refLon=None)

A convenience routine to plot the H2 dissociation map.

Parameters:

refLon (float, optional) – The centre longitude used to rotate the map.

Returns:

The figure containing the plot.

Return type:

figure

plot_map(refLon=None)

A convenience routine to plot the temperature map

Parameters:

refLon (float, optional) – The centre longitude used to rotate the map.

Returns:

The figure containing the plot.

Return type:

figure

set_values(values, time=None, dissValues=None)

Set the temperature map.

Parameters:

• values (ndarray) – The map temperatures (in K) with a size of self.npix.

• time (float, optional) – Time of map in days.

• dissValues (ndarray, optional) – The H2 dissociation fraction values for the map.

Bell_EBM.Planet module

class Bell_EBM.Planet.Planet(plType='gas', rad=71492000.0, mass=1.8981245973360505e+27, a=4487936121.0, Porb=None, Prot=None, inc=90.0, t0=0.0, e=0.0, Omega=270.0, argp=90, obliq=0.0, argobliq=0.0, vWind=0.0, albedo=0.0, cp=None, cpParams=None, mlDepth=None, mlDensity=None, T_exponent=4.0, emissivity=1.0, trasmissivity=0.0, internalFlux=0.0, instRedistFrac=0.0, nlat=16, nlon=None)

Bases: object

A planet.

albedo

The planet’s Bond albedo.

Type:

float

cpParams

Any parameters to be passed to cp if using the bell2018 LTE H2+H mix cp

Type:

iterable, optional

C

The planet’s heat capacity in J/m^2/K.

Type:

float, optional

emissivity

The emissivity of the emitting layer (between 0 and 1).

Type:

float

g

The planet’s surface gravity in m/s^2.

Type:

float

instRedistFrac

The fraction of flux that is instantly redistributed across the entire planet.

Type:

float

internalFlux

The planet’s internal heating flux in W/m^2.

Type:

float

orbit

The planet’s orbit.

Type:

Bell_EBM.KeplerOrbit

trasmissivity

The trasmissivity of the emitting layer (between 0 and 1).

Type:

float

T_exponent

The exponent which determinges the rate at which the planet cools (4 for blackbody cooling, 1 for Newtonian cooling) when calculating Fout with bolo=True.

Type:

float

Fout(T=None, bolo=True, wav=4.5e-06, lookup=True)

Calculate the instantaneous outgoing flux.

Parameters:

• T (ndarray) – The temperature (if None, use self.map.values).

• bolo (bool, optional) – Determines whether computed flux is bolometric (True, default) or wavelength dependent (False).

• wav (float, optional) – The wavelength to use if bolo==False.

• lookup (bool, optional) – Use lookup tables to speed up computation of bolometric flux (default=True).

Returns:

The emitted flux in the same shape as T.

Return type:

ndarray

Fp_vis(t, T=None, TA=None, bolo=True, wav=4.5e-06, lookup=True)

Calculate apparent outgoing planetary flux (used for making phasecurves).

Weight flux by visibility/illumination kernel, assuming the star/observer are infinitely far away for now.

Parameters:

• t (ndarray) – The time in days.

• T (ndarray, optional) – The temperature (if None, use self.map.values).

• TA (ndarray, optional) – The true anomaly in radians.

• bolo (bool, optional) – Determines whether computed flux is bolometric (True, default) or wavelength dependent (False).

• wav (float, optional) – The wavelength to use if bolo==False

• lookup (bool, optional) – Use lookup tables to speed up computation of bolometric flux (default=True).

Returns:

The apparent emitted flux. Has shape (t.size, self.map.npix).

Return type:

ndarray

property Porb

The planet’s orbital period in days.

Type:

float

property Prot

The planet’s rotational period in days.

Type:

float

property absorptivity

The fraction of flux absorbed by the planet.

Read-only.

Type:

float

property cp

The planet’s isobaric specific heat capacity in J/kg/K.

Changing the planet’s cp may update planet.C

Type:

float or callable

property map

The planet’s temperature map.

Type:

Bell_EBM.Map

property mass

The planet’s mass in kg.

Changing the planet’s mass will update planet.g and possibly planet.mlDensity and planet.C

Type:

float

property mlDensity

The density of the planet’s mixed layer

In kg/m^3 if rock/water models or the inverse of the planet’s surface gravity (in s^2/m) for gas/bell2018 models.

Changing the planet’s mlDensity may update planet.C

Type:

float

property mlDepth

The depth of the planet’s mixed layer.

In units of m for rock/water models, or Pa for gas/bell2018 models.

Changing the planet’s mlDepth may update planet.C

Type:

float

property plType

The planet’s composition.

Type:

str

plot_H2_dissociation(dissMap=None, refLon=None)

A convenience routine to plot the planet’s H2 dissociation map.

Parameters:

• dissMap (ndarray, optional) – The H2 dissociation fraction values for the map (if None, use self.map.dissValues).

• refLon (float, optional) – The centre longitude used to rotate the map.

Returns:

The figure containing the plot.

Return type:

figure

plot_map(tempMap=None, refLon=None)

A convenience routine to plot the planet’s temperature map.

Parameters:

• tempMap (ndarray) – The temperature map (if None, use self.map.values).

• refLon (float, optional) – The centre longitude used to rotate the map.

Returns:

The figure containing the plot.

Return type:

figure

property rad

The planet’s radius if m.

Changing the planet’s radius will update planet.g and possibly planet.mlDensity and planet.C

Type:

float

property t0

The planet’s linear ephemeris in days.

Type:

float

property vWind

The planet’s windspeed in m/s.

Type:

float

weight(t, TA=None, refPos='SSP')

Calculate the weighting of map pixels.

Weight flux by visibility/illumination kernel, assuming the star/observer are infinitely far away for now.

Parameters:

• t (ndarray) – The time in days.

• TA (ndarray, optional) – The true anomaly in radians.

• refPos (str, optional) – The reference position; SSP (sub-stellar point) or SOP (sub-observer point).

Returns:

The weighting of map mixels at time t. Has shape (t.size, self.map.npix).

Return type:

ndarray

Bell_EBM.Star module

class Bell_EBM.Star.Star(teff=5778.0, rad=1.0, mass=1.0)

Bases: object

A star.

teff

The star’s effective temperature in K.

Type:

float

rad

The star’s radius in solar radii.

Type:

float

mass

The star’s mass in solar masses.

Type:

float

Fstar(bolo=True, tBright=None, wav=4.5e-06)

Calculate the stellar flux for lightcurve normalization purposes.

Parameters:

• bolo (bool, optional) – Determines whether computed flux is bolometric (True, default) or wavelength dependent (False).

• tBright (ndarray) – The brightness temperature to use if bolo==False.

• wav (float, optional) – The wavelength to use if bolo==False.

Returns:

The emitted flux (in Watts) in the same shape as T.

Return type:

ndarray

Bell_EBM.StarPlanetSystem module

class Bell_EBM.StarPlanetSystem.System(star=None, planet=None, neq=False)

Bases: object

A Star+Planet System.

star

The host star.

Type:

Bell_EBM.Star

planet

The planet.

Type:

Bell_EBM.Planet

Fin(t=0, TA=None, bolo=True, tStarBright=None, wav=4.5e-06)

Calculate the instantaneous incident flux.

Parameters:

• t (ndarray, optional) – The time in days.

• TA (ndarray, optional) – The true anomaly in radians.

• bolo (bool, optional) – Determines whether computed flux is bolometric (True, default) or wavelength dependent (False).

• tStarBright (ndarray) – The stellar brightness temperature to use if bolo==False.

• wav (float, optional) – The wavelength to use if bolo==False.

Returns:

The instantaneous incident flux.

Return type:

ndarray

Firr(t=0.0, TA=None, bolo=True, tStarBright=None, wav=4.5e-06)

Calculate the instantaneous irradiation.

Parameters:

• t (ndarray, optional) – The time in days.

• TA (ndarray, optional) – The true anomaly in radians.

• bolo (bool, optional) – Determines whether computed flux is bolometric (True, default) or wavelength dependent (False).

• tStarBright (ndarray) – The stellar brightness temperature to use if bolo==False.

• wav (float, optional) – The wavelength to use if bolo==False.

Returns:

The instantaneous irradiation.

Return type:

ndarray

ODE_EQ(t, T, dt, TA=None, Fin=None, lookup=True)

The derivative in temperature with respect to time.

This function neglects for the timescale of dissociation/recombination for bell2018 planets.

Parameters:

• t (float) – The time in days.

• T (ndarray) – The temperature map with shape (self.planet.map.npix).

• dt (float) – The time step in days.

• TA (ndarray, optional) – The true anomaly in radians (much faster to compute if provided).

• Fin (ndarray, optional) – The incident stellar flux for each pixel.

• lookup (bool, optional) – Use lookup tables to speed up computation of bolometric flux (default=True).

Returns:

The derivative in temperature with respect to time.

Return type:

ndarray

ODE_NEQ(t, T, dt, TA=None, Fin=None, lookup=True)

The derivative in temperature with respect to time.

This function accounts for the timescale of dissociation/recombination for bell2018 planets.

Parameters:

• t (float) – The time in days.

• T (ndarray) – The temperature map with shape (self.planet.map.npix).

• dt (float) – The timestep in days.

• TA (ndarray, optional) – The true anomaly in radians (much faster to compute if provided).

• Fin (ndarray, optional) – The incident stellar flux for each pixel.

• lookup (bool, optional) – Use lookup tables to speed up computation of bolometric flux (default=True).

Returns:

The derivative in temperature with respect to time.

Return type:

ndarray

get_phase(t)

Get the orbital phase.

Parameters:

t (ndarray) – The time in days.

Returns:

The orbital phase.

Return type:

ndarray

get_phase_eclipse()

Get the orbital phase of eclipse.

Returns:

The orbital phase of eclipse.

Return type:

float

get_phase_periastron()

Get the orbital phase of periastron.

Returns:

The orbital phase of periastron.

Return type:

float

get_phase_transit()

Get the orbital phase of transit.

Returns:

The orbital phase of transit.

Return type:

float

get_teq(t=0)

Get the planet’s equilibrium temperature.

Parameters:

t (ndarray, optional) – The time in days.

Returns:

The planet’s equilibrium temperature at time(s) t.

Return type:

ndarray

get_tirr(t=0.0)

Get the planet’s irradiation temperature.

Parameters:

t (ndarray, optional) – The time in days.

Returns:

The planet’s irradiation temperature at time(s) t.

Return type:

ndarray

invert_lc(fp_fstar, bolo=True, tStarBright=None, wav=4.5e-06)

Invert the fp/fstar phasecurve into an apparent temperature phasecurve.

Parameters:

• fp_fstar (ndarray) – The observed planetary flux normalized by the stellar flux.

• bolo (bool, optional) – Determines whether computed flux is bolometric (True, default) or wavelength dependent (False).

• tBright (ndarray) – The brightness temperature to use if bolo==False.

• wav (float, optional) – The wavelength to use if bolo==False.

Returns:

The apparent, disk-integrated temperature.

Return type:

ndarray

lightcurve(t=None, T=None, TA=None, bolo=True, tStarBright=None, wav=4.5e-06, allowReflect=True, allowThermal=True, lookup=True)

Calculate the planet’s lightcurve (ignoring any occultations).

Parameters:

• t (ndarray, optional) – The time in days. If None, will use 1000 time steps around orbit.

• T (ndarray, optional) – The temperature map (either shape (1, self.planet.map.npix) and constant over time or shape is (t.shape, self.planet.map.npix). If None, use self.planet.map.values instead (default).

• TA (ndarray, optional) – The true anomaly in radians.

• bolo (bool, optional) – Determines whether computed flux is bolometric (True, default) or wavelength dependent (False).

• tStarBright (ndarray) – The stellar brightness temperature to use if bolo==False.

• wav (float, optional) – The wavelength to use if bolo==False.

• allowReflect (bool, optional) – Account for the contribution from reflected light.

• allowThermal (bool, optional) – Account for the contribution from thermal emission.

• lookup (bool, optional) – Use lookup tables to speed up computation of bolometric flux (default=True).

Returns:

The observed planetary flux normalized by the stellar flux.

Return type:

ndarray

plot_lightcurve(t=None, T=None, TA=None, bolo=True, tStarBright=None, wav=4.5e-06, allowReflect=False, allowThermal=True, lookup=True)

A convenience plotting routine to show the planet’s phasecurve.

Parameters:

• t (ndarray, optional) – The time in days with shape (t.size,1). If None, will use 1000 time steps around orbit.

• T (ndarray, optional) – The temperature map in K with shape (1, self.planet.map.npix) if the map is constant or (t.size,self.planet.map.npix). If None, use self.planet.map.values instead.

• TA (ndarray, optional) – The true anomaly in radians.

• bolo (bool, optional) – Determines whether computed flux is bolometric (True, default) or wavelength dependent (False).

• tBright (ndarray) – The brightness temperature to use if bolo==False.

• wav (float, optional) – The wavelength to use if bolo==False.

• allowReflect (bool, optional) – Account for the contribution from reflected light.

• allowThermal (bool, optional) – Account for the contribution from thermal emission.

• lookup (bool, optional) – Use lookup tables to speed up computation of bolometric flux (default=True).

Returns:

The figure containing the plot.

Return type:

figure

plot_tempcurve(t=None, T=None, TA=None, bolo=True, tStarBright=None, wav=4.5e-06, allowReflect=False, allowThermal=True, lookup=True)

A convenience plotting routine to show the planet’s phasecurve in units of temperature.

Parameters:

• t (ndarray, optional) – The time in days with shape (t.size,1). If None, will use 1000 time steps around orbit. Must be provided for eccentric planets.

• T (ndarray, optional) – The temperature map in K with shape (1, self.planet.map.npix) if the map is constant or (t.size,self.planet.map.npix). If None, use self.planet.map.values instead. Must be provided for eccentric planets.

• TA (ndarray, optional) – The true anomaly in radians.

• bolo (bool, optional) – Determines whether computed flux is bolometric (True, default) or wavelength dependent (False).

• tBright (ndarray) – The brightness temperature to use if bolo==False.

• wav (float, optional) – The wavelength to use if bolo==False.

• allowReflect (bool, optional) – Account for the contribution from reflected light.

• allowThermal (bool, optional) – Account for the contribution from thermal emission.

• lookup (bool, optional) – Use lookup tables to speed up computation of bolometric flux (default=True).

Returns:

The figure containing the plot.

Return type:

figure

run_model(T0=None, t0=0.0, t1=None, dt=None, verbose=True, intermediates=False, progressBar=False, minTemp=0, lookup=True)

Evolve the planet’s temperature map with time.

Parameters:

• T0 (ndarray) – The initial temperature map with shape (self.planet.map.npix). If None, use self.planet.map.values instead (default).

• t0 (float, optional) – The time corresponding to T0 (default is 0).

• t1 (float, optional) – The end point of the run (default is 1 orbital period later).

• dt (float, optional) – The time step used to evolve the map (default is 1/100 of the orbital period).

• verbose (bool, optional) – Output comments of the progress of the run (default = False)?

• intermediates (bool, optional) – Output the map from every time step? Otherwise just returns the last step.

• progressBar (bool, optional) – Show a progress bar for the run (nice for long runs).

• minTemp (float, optional) – The minimum allowable temperature (can be used to vaguely mimick internal heating).

• lookup (bool, optional) – Use lookup tables to speed up computation of bolometric flux (default=True).

Returns:

A list of 2 ndarrays containing the time and map of each time step.

Return type:

list

Module contents