params.py

from aart_func import *

#BH's Spin
spin_case=15/16

#Observer's inclination  
i_case=17

# Distance to the BH in meters (default: M87)
dBH=5.214795112e23  
# BH mass-to-distance ratio (default: 1/psi= 6.2e9 Kg)
psi=1.07473555940836 
#Observer's distance in units of M
D_obs=10000 

#Velocity Profile for the gas

#The CosAngle (cosine of the emission angle) currently just works for Keplerian velocities
#Sub-Kepleniarity param
sub_kep=1.0;
#Radial velocity param
betar=1.0;
#Angular velocity param
betaphi=1.0;

# If equal to 1, the radon cuts profiles will be stored   
radonfile=0
 
#For the Image resolution in the Bardeen coordinates
#Limits for the image [M]. It should coincide with the inoisy if used.
#If equal to 1, the sizes of the grids will be equal and an image can be computed
#by summing the contributions    
p_image=1
limits=15
#Resolution for the n=0 image [M]
dx0 = 0.02
#Resolution for the n=1 image [M]
dx1 = 0.02
#Resolution for the n=2 image [M]
dx2 = 0.02

# Projection angles for the radon transformation
radonangles=[0,90]

# inoisy movie file name
i_fname="inoisy_256_128_30_1000_5.00_0.10_0.9400_1.00_1.00_1.00_0.349_137.0_137.0_1662.0.h5"

# inoisy initial time frame for single images
i_frame=0

# Initial and final times in units of M
i_tM=0  
#Makes sense when is less than the inosy temporal length 
f_tM=1000
#Number of snapshots in that range    
snapshots=100

#When False, several quantities will be stored in the resulting files
smallfiles=True

#ISCO and horizon values
isco = rms(spin_case)
horizon=1+np.sqrt(1-spin_case**2)

#Magnetic field parametrs
cr=0.0
cphi=1.0

# Useful for disk visualizations or when studying truncated disks.
# 0: Neglected
# 1: Radii computed up to thar radius
# 2: Adds 5M to r_cutoff for interpolation purposes. 
imag_cut=0
# Cutoff radius   
r_cutoff=20

#The power of the redshift factor
gfactor=3

# Max baseline in G\lambda

# Number of points in the critical curve 
npointsS=100    

#For the parallel generation of images (movies) #Not implemented yet
nthreads=4

#Observer's inclination in radians
thetao=i_case*np.pi/180
#Disk's inclination  
#Current version is just implemented for equatorial models   
i_disk=90    
thetad=i_disk*np.pi/180

Gc=6.67e-11 # G constant [m^3 kg^-1 s^-2]
cc= 2.99792458e8 # c constant [m/s]
Msc=1.988435e30 # Solar Mass [Kg]

MMkg= 6.047999383e9*psi*Msc # [Kg] 6.5 solar mass
MM=MMkg *Gc/cc**2 # Mass of the BH in meters, i.e., for M87(psi*6.2*10^9) psi ("Best fit") Solar Masses 

# Size of the real image in meters
sizeim_Real=(limits)*MM 
#1 microarcsec in radians
muas_to_rad = np.pi/648000 *1e-6 
fov_Real=np.arctan(sizeim_Real/(dBH))/muas_to_rad #muas

#Path where the results will be stored
path = './Results/'

# Create a directory for the results
isExist = os.path.exists(path)
if not isExist:
    os.makedirs(path)
    print("A directory (Results) was created to store the results")

'''
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Permission is hereby granted, free of charge, to any person obtaining a copy of this 
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'''