- I want to use the spectrum from POWR models of the O2 star
- And find the ionization structure for simple models, assuming constant density
- Compare with He++/He+ structure, and also Ar+++/Ar++ (and Ne++, O++ too to a certain extent)
- Look up how I did this for the Raman project
- The best example seems to be Combine fine and coarse and make them suitable for Cloudy
- For this project, the coarse SEDs should be sufficient,
- but I still need to convert them to Cloudy’s expected units
- and maybe I should check for duplicates while I am at it
from pathlib import Path
import numpy as np
datapath = Path("../stars/powr/seds")
infiles = datapath.glob("*_sed.txt")
wavtot = None
for infile in infiles:
wav, flam = np.loadtxt(infile, unpack=True)
# Make sure no repeated entries
wav_unique = np.sort(list(set(wav)))
flam_unique = np.interp(wav_unique, wav, flam)
# Write out a version to be used with Cloudy's "table SED" command
# Energy in Rydbergs
e_ryd = 1e8/(1.09737315685e5 * 10**wav_unique)
# Use that Fnu = (lam/nu) Flam = (lam**2 / c) Flam and don't worry
# about the normalization
Fnu = 10**(flam_unique + 2*wav_unique)
outfile = str(infile).replace("_sed.txt", ".sed")
# Write out the sed in fixed-width 14-character columns
header = f"{'E, Ryd':14s}{'F_nu':14s}"
data = list(zip(e_ryd[::-1], Fnu[::-1]))
np.savetxt(outfile, data, header=header, fmt="%14.7e")
Copy SED files to cloudy model folder
cp -pv ../stars/powr/seds/*.sed ../cloudy/models+ The files "*_sed.txt" are the originals downloaded from POWR website
+ The columns are log10(lambda) and log10(F_lambda)
+ The files "*.sed" have been converted for use with Cloudy's "table SED" command
+ The columns are E, Rydbergs and F_nu
- From Which are the most important stars for mYSO C?
- Bolometric luminosity: 1.1e6 Lsun = 4.202e39 erg/s
- Update [2024-03-14 Thu] Add the infrared lines and continuum bands to the Cloudy output
title Walborn 3 in SMC-N66 / NGC 346, bow shock, n = 10 pcc
# Density of 10 pcc
hden 1.00
constant density
magnetic field -5.3 gauss
<<cloudy-w3-radiation>>
<<cloudy-w3-common-physical>>
<<cloudy-saves>>
title Walborn 3 in SMC-N66 / NGC 346, bow shock, constant P, n0 = 10 pcc
# Density of 10 pcc
hden 1.00
constant pressure
magnetic field -5.3 gauss
<<cloudy-w3-radiation>>
<<cloudy-w3-common-physical>>
<<cloudy-saves>>
- The B field has also been increased by sqrt(3) to maintain the same Alfven speed
title Walborn 3 in SMC-N66 / NGC 346, bow shock, constant P, n0 = 30 pcc
# Density of 30 pcc
hden 1.48
constant pressure
magnetic field -5.54 gauss
<<cloudy-w3-radiation>>
<<cloudy-w3-common-physical>>
<<cloudy-saves>>
title Walborn 3 in SMC-N66 / NGC 346, bow shock, constant P, n0 = 10 pcc, up to 8 pc
# Density of 10 pcc
hden 1.00
constant pressure
magnetic field -5.3 gauss
stop radius 19.39
<<cloudy-w3-radiation>>
<<cloudy-w3-common-physical>>
<<cloudy-saves>>
title Walborn 3 in SMC-N66 / NGC 346, bow shock, constant P, n0 = 10 pcc, up to 8 pc
# Density of 10 pcc
hden 0.699
constant pressure
magnetic field -5.45 gauss
stop radius 19.39
<<cloudy-w3-radiation>>
<<cloudy-w3-common-physical>>
<<cloudy-saves>>
title Walborn 3 in SMC-N66 / NGC 346, bow shock, constant P, n0 = 100 pcc, up to 8 pc
# Density of 100 pcc
hden 2.00
constant pressure
magnetic field -4.8 gauss
stop radius 19.39
<<cloudy-w3-radiation>>
<<cloudy-w3-common-physical>>
<<cloudy-saves>>
title Walborn 3 in SMC-N66 / NGC 346, bow shock, constant P, n0 = 100 pcc, up to 8 pc
# Density of 50 pcc
hden 1.699
constant pressure
magnetic field -4.95 gauss
stop radius 19.39
<<cloudy-w3-radiation>>
<<cloudy-w3-common-physical>>
<<cloudy-saves>>
title Walborn 3 in SMC-N66 / NGC 346, bow shock, power law r^-1, n0 = 10 pcc, up to 8 pc
# Density of 10 pcc
hden 1.00, power = -1
magnetic field -5.3 gauss
stop radius 19.39
<<cloudy-w3-radiation>>
<<cloudy-w3-common-physical>>
<<cloudy-saves>>
# POWR SMC 50000 K model with standard wind
table SED "smc-ob-i_50-42.sed"
# Bolometric luminosity of 1.1e6 Lsun
luminosity total 39.62
# Add 10 L_sun of 1e6 K x-rays
brems 6
luminosity total 34.6
# And general Milky Way backgrounds
cmb
table ism
cosmic rays, background
- We will try constant density to start with
- Start with 10 pcc, but could be higher
- But leave this to the specific models
- Inner radius is about 4 arcsec, so 1.2 pc = 3.703e+18 cm
- 18.57 on log scale
- Magnetic field
- Assume Alfven speed of 3 km/s
- B / (4 pi ρ)1/2 = 3 km/s
- B = 3 1.0e5 sqrt(4 pi 10 2e-24) = 4.75e-6 G
- -5.323 on log10 scale
- Abundances are largely from Valerdi:2019a
# 1.2 pc
radius 18.57
turbulence 5 km/s
iterate
init file="ism.ini"
# Approximation to SMC abundances
abundances HII no grains
# 0.3x ISM grain abundance
grains ISM 0.3
# Particular elements from Valerdi+ 2019
# Note that scale is log10 wrt H (12 less than conventional value)
element abundance helium -1.084
element abundance nitrogen -5.39
element abundance oxygen -3.81
element abundance neon -4.52
element abundance sulphur -5.56
element abundance argon -6.18
element abundance chlorine -6.53
# All other elements get scaled to ISM x 0.3
element scale factor carbon 0.3
element scale factor magnesium 0.3
element scale factor silicon 0.3
element scale factor phosphorus 0.3
element scale factor iron 0.3
element scale factor nickel 0.3
- Unlike in the Raman project, I am not interested in the PDR or the FUV pumping lines
- But I am interested in getting all the observed optical lines
- Update [2024-03-14 Thu] I have added a whole bunch of continuum bands in the mid-infrared for comparison with the Spitzer data
save overview last ".ovr"
save continuum last ".cont"
save pressure last ".pre"
save cooling last ".cool"
save heating last ".heat"
save physical conditions last ".phys"
save hydrogen lya last ".lya"
save lines, emissivity last ".emis"
He 2 4685.70
O 1 6300.30
O 2 7319.99
O 2 7318.92
O 3 4363.21
O 3 5006.84
Ar 3 7135.79
Ar 4 4711.26
Ar 4 4740.12
Ar 4 7332.15
Ar 3 7751.11
Ne 3 3868.76
Ne 4 4724.17
S 3 6312.06
S 3 9068.62
H 1 4861.33
H 1 6562.82
Ca B 6562.82
Blnd 5875.66A
Ne 3 15.5509m
Ne 2 12.8101m
S 4 10.5076m
S 3 18.7078m
S 3 33.4704m
Si 2 34.8046m
Ar 3 8.98898m
PAHC 6.90000m
PAHC 10.9000m
PAH 11.3000m
PAHC 14.1000m
nFnu 15.6901m
nFnu 19.6199m
nFnu 24.7829m
nFnu 30.8695m
nFnu 41.2152m
nFnu 60.8322m
IRAC 3.60000m
IRAC 4.50000m
IRAC 5.80000m
IRAC 8.00000m
F12 12m
F25 25m
MIPS 24m
PAC1 70m
PAC2 100m
PAC3 160m
end of lines
save lines, array ".lina" last, units microns
save radius last ".rad"
# Everything about grains
save grain abundance last ".gabun"
save grain charge last ".gcharge"
save grain continuum last ".gcont"
save grain drift velocity last ".gdrift"
save grain potential last ".gpot"
save grain temperature last ".gtemp"
# Ionization structure per element
save element carbon last ".C"
save element nitrogen last ".N"
save element oxygen last ".O"
save element sulphur last ".S"
save element argon last ".Ar"
save element neon last ".Ne"
save element silicon last ".Si"
save element chlorine last ".Cl"
- These are in notebook
- It is hard to get the [Ar IV] to fall off on the right scale
- We can maybe do it with a constant density model with n = 50
- Or we can have a density that falls with radius