https://github.com/sevenian3/ChromaStarPy
Tip revision: 103d3d0df6d9574c49818f149e1cae8100455d10 authored by Ian Short on 06 July 2023, 18:09:20 UTC
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Tip revision: 103d3d0
Input.py
#
#
#Custom filename tags to distinguish from other runs
project = "SunEarth"
runVers = "Test"
#Project specific notes:
# Test case:
# Star: Sun
# Spectrum: Na I D region
# Lightcurve: Earth, in plane of ecliptic
#Default plot
#Select ONE only if plotting 'inline' -
makePlotStruc = True
makePlotSED = True
makePlotSpec = True
makePlotLDC = True
makePlotFT = True
makePlotTLA = True
makePlotTrans = True
makePlotPPress = False
#Chemical species for partial rpessure plot:
plotSpec = "H"
#Spectrum synthesis mode
# - uses model in Restart.py with minimal structure calculation
specSynMode = True
if (specSynMode):
runVers += "SS"
#Model atmosphere
teff = 5777.0 #, K
logg = 4.44 #, cgs
log10ZScale = -0.0 # [A/H]
massStar = 1.00 #, solar masses
xiT = 1.0 #, km/s
logHeFe = 0.0 #, [He/Fe]
logCO = 0.0 #, [C/O]
logAlphaFe = 0.0 #, [alpha-elements/Fe]
#Spectrum synthesis
lambdaStart = 588.5 #, nm
lambdaStop = 589.5 #, nm
fileStem = project + "-"\
+ str(round(teff, 7)) + "-" + str(round(logg, 3)) + "-" + str(round(log10ZScale, 3))\
+ "-" + str(round(lambdaStart, 5)) + "-" + str(round(lambdaStop, 5))\
+ "-" + runVers
lineThresh = -3.0 #, min log(KapLine/kapCnt) for inclusion at all - areally, being used as "lineVoigt" for now
voigtThresh = -3.0 #, min log(KapLine/kapCnt) for treatment as Voigt - currently not used - all lines get Voigt
logGammaCol = 0.5 # Logarithmic VdW damping enhancement
logKapFudge = 0.0 # continuum opacity fudge factor
macroV = 1.0 #, macroscopic broadening dispersion km/s
rotV = 2.0 #, equatorial surface rotational velocity km/s
rotI = 90.0 #, inclination of rotational axis AND orbital axis degrees
RV = 0.0 #, system radial velocity km/s
vacAir = "vacuum" # wavelength scale ('air' OR 'vacuum')
sampling = "fine" # density of freq points in spectrum synthesis ('fine' is useful, 'coarse' for quick checking)
#Performance vs realism
nOuterIter = 12 #, no of outer Pgas(HSE) - EOS - kappa iterations
nInnerIter = 12 #, no of inner (ion fraction) - Pe iterations
ifMols = 1 #, whether to include TiO JOLA bands in synthesis
#Gaussian filter for limb darkening curve (LDC), fourier transform (FT)
diskLambda = 500.0 #, Band centre wavelength nm
diskSigma = 0.01 #, Band dispersion nm
#Two-level atom and spectral line
#Example: NaI D lambda 5896:
userLam0 = 589.592 #, nm
userA12 = 6.24 #, A_12 logarithmic abundance = log_10(N/H_H) = 12
userLogF = -0.495 #, log(f) oscillaotr strength // saturated line
userStage = 0 #, ionization stage of user species (0 (I) - 3 (IV)
userChiI1 = 5.139 #, ground state chi_I, eV
userChiI2 = 47.29 #, 1st ionized state chi_I, eV
userChiI3 = 71.62 #, 2nd ionized state chi_I, eV
userChiI4 = 98.94 #, 3rd ionized state chi_I, eV
userChiL = 0.0 #, lower atomic E-level, eV
userGw1 = 2 #, ground state state. weight or partition fn (stage I) - unitless
userGw2 = 1 #, ground state state. weight or partition fn (stage II) - unitless
userGw3 = 1 #, ground state state. weight or partition fn (stage III) - unitless
userGw4 = 1 #, ground state state. weight or partition fn (stage IV) - unitless
userGwL = 2 #, lower E-level state. weight - unitless
userMass = 22.9 #, amu
userLogGammaCol = 1.0 #, log_10 Lorentzian broadening enhancement factor
#Planetary transit parameters for transit light curve modelling
# ** Also depends on rotI chosen above!!
# Oribital period is not a free parameter - it is set by the
# size of the orbit and the planet's mass by basic form of
#Kepler's 3rd law
rJupiter = 11.21 # Earth radii - handy reference
ifTransit = True # set to True if we want an exoplanet lightcurve
#Data source: Wikipedia for now...
rOrbit = 1.00 # AU
rPlanet = 1.00 #Earth radii
#mPlanet = 1.0 #Earth masses #not needed (yet?)