Wagle+ in preparation claim that WMbasic gives better fit to [Ne III] lines.
Trapezium_WMbasic shows this
Veusz file and pdf compare these two.
* * *
The original form came from Will Henney in email of
2012 Dec 5. His notes follow:
> Stellar parameters for C, A, D are from Simón-Díaz \cite{2006A&A…448..351S}
> I originally had th1B as a B2V star, which should be cooler than what Gary had (28kK and 10**4.4 Lsun), but I can't find the provenance of this
> actually th1B (BM Ori) is a quintuple system: see SIMBAD record
> SIMBAD says primary is B1V citing \cite{Close:2003}, but that paper does not mention spectral types at all. I suspect this is a confusion with B1, B2, etc being the designations of the quintuple components
> \cite{Weigelt:1999} find a B3 spectral type for the primary (B1) with log L = 3.25 and T = 18000
> B2, B3, and B4 are all lower mass, but B5 has mass similar to B1 accoding to \cite{Weigelt:1999}. However, this must be a mistake: according to \cite{Abt:1991}, who detect B1 and B5 as an eclipsing spectroscopic binary, the mass ratio is 0.3, implying that B5 has a mass of only 2 Msun..
> th1C is a triple system \cite{Lehmann:2010a}
> \cite{Schertl:2003} have broad constraints on the parameters of C2 (dark gray line in their Fig 4). If we take the middle of this range, we get a giantish B3IV star: log L = 3.8, T = 17000, M = 9 Msun, age much less than 1 Myr.
> We can work out the surface gravity:
> g = G M / R2 = G M 4 pi sigma T4 / L = 6.673e-8 9 1.989e33 4 pi 5.6703e-5 17000**4 / 10**3.8 3.82e33 = 2950 cm/s2 => log g = 3.5
> [X] We should check these parameters against \cite{Lehmann:2010a}, who say 12 Msun in their abstract. The article itself is not freely available -grab it when I get back to work
> If we use the same evo tracks as in \cite{Schertl:2003}, then this would imply B2IV with log L = 4.0, T = 21000
> So, after checking out the Lehman article, it seems the 12 Msun is robust, since it is based on orbital solution. The translation to luminosity and Teff is rather more speculative.
> In fact, according to \cite{Kraus:2007}, the companion is O9.5V with Teff = 32000, log L = 4.68. This is also consistent with the Schertl tracks, but it is assuming 15.5 Msun.
> If we instead use 12 Msun as the best mass estimate \cite{Lehmann:2010a}, then we would get log L = 4.2, Teff = 25,000
> Recalculate surface gravity for new parameters
> g = G M / R2 = G M 4 pi sigma T4 / L = 6.673e-8 12 1.989e33 4 pi 5.6703e-5 25000**4 / 10**4.2 3.82e33 = 7322 cm/s2 => log g = 3.86
>
> 2014 May 06, changed some tlusty stars to WMBasic - had used tlusty for all stars originally. WMBasic produces better agreement with H II region optical emission, especially [Ne III]
> Using this new solution for th1C2 changes the broadband ratios by about 5%.
Wagle+ in preparation claim that WMbasic gives better fit to [Ne III] lines.
Trapezium_WMbasic shows this
Veusz file and pdf compare these two.
***************************
The original form came from Will Henney in email of
2012 Dec 5. His notes follow:
Stellar parameters for C, A, D are from Simón-Díaz \cite{2006A&A…448..351S}
I originally had th1B as a B2V star, which should be cooler than what Gary had (28kK and 10**4.4 Lsun), but I can't find the provenance of this
actually th1B (BM Ori) is a quintuple system: see SIMBAD record
SIMBAD says primary is B1V citing \cite{Close:2003}, but that paper does not mention spectral types at all. I suspect this is a confusion with B1, B2, etc being the designations of the quintuple components
\cite{Weigelt:1999} find a B3 spectral type for the primary (B1) with log L = 3.25 and T = 18000
B2, B3, and B4 are all lower mass, but B5 has mass similar to B1 accoding to \cite{Weigelt:1999}. However, this must be a mistake: according to \cite{Abt:1991}, who detect B1 and B5 as an eclipsing spectroscopic binary, the mass ratio is 0.3, implying that B5 has a mass of only 2 Msun..
th1C is a triple system \cite{Lehmann:2010a}
\cite{Schertl:2003} have broad constraints on the parameters of C2 (dark gray line in their Fig 4). If we take the middle of this range, we get a giantish B3IV star: log L = 3.8, T = 17000, M = 9 Msun, age much less than 1 Myr.
We can work out the surface gravity:
g = G M / R2 = G M 4 pi sigma T4 / L = 6.673e-8 9 1.989e33 4 pi 5.6703e-5 17000**4 / 10**3.8 3.82e33 = 2950 cm/s2 => log g = 3.5
[X] We should check these parameters against \cite{Lehmann:2010a}, who say 12 Msun in their abstract. The article itself is not freely available -grab it when I get back to work
If we use the same evo tracks as in \cite{Schertl:2003}, then this would imply B2IV with log L = 4.0, T = 21000
So, after checking out the Lehman article, it seems the 12 Msun is robust, since it is based on orbital solution. The translation to luminosity and Teff is rather more speculative.
In fact, according to \cite{Kraus:2007}, the companion is O9.5V with Teff = 32000, log L = 4.68. This is also consistent with the Schertl tracks, but it is assuming 15.5 Msun.
If we instead use 12 Msun as the best mass estimate \cite{Lehmann:2010a}, then we would get log L = 4.2, Teff = 25,000
Recalculate surface gravity for new parameters
g = G M / R2 = G M 4 pi sigma T4 / L = 6.673e-8 12 1.989e33 4 pi 5.6703e-5 25000**4 / 10**4.2 3.82e33 = 7322 cm/s2 => log g = 3.86
2014 May 06, changed some tlusty stars to WMBasic - had used tlusty for all stars originally. WMBasic produces better agreement with H II region optical emission, especially [Ne III]
Using this new solution for th1C2 changes the broadband ratios by about 5%.
<p>This documents the data files included in the Cloudy data distribution.
Those instructions for setting up the code are on the
<ahref="http://www.nublado.org">web site</a>.</p>
<p>Three types of files are present in this directory. </p>
<p><strong><em>*.ini</em></strong> These are files that are used to set up Cloudy. You can change these files to alter the code's default behavior. These can, for instance, change the continuum resolution or add
new entries into the main emission-line output.</p>
<p><strong><em>*.da</em></strong>t These are the foundation atomic/molecular data files that are needed for the code to operate. Do not change these files.</p>
<p><strong><em>*.in</em></strong> These are input scripts that are used to compile various
helper files such as stellar atmospheres or types of grains. </p>
<hr>
<h2><aname="Compiling ancillary files with the *.in input files">Compiling
ancillary files with the *.in input files</a></h2>
<p>The download includes all the files you will need to get Cloudy running.
The download does not include the stellar continua file that are needed for the
table stars command to work. The web site describes how to set up these continua
and this only needs to be done if you want to use the table stars command.
Several input files (names like compile*.in) are examples of compiling some of
the stellar continua.</p>
<h3>(Possibly) compiling the size-distributed grains</h3>
<p>It is easy to create new grain tipes. Compiled opacities are already included in the data
files (the *.opc files), so nothing need be done if you are happy with the
default setup. They would need to be recompiled if you change the
energy grid of the code, or wish to use a different grain refractive index or size
distribution. Distributed grains are new in C96 and were added in collaboration
with Peter van Hoof and Peter G. Martin. These use optical properties for
each grain material (the *.rfi files) and size distribution files (the *.szd
files) to create grain opacities (the *.opc files) that are a function of grain
material and size. The code can then do a more realistic simulation of the grain
emission and physics </p>
<p><fontsize="3"><kbd><strong>compilegrains.in</strong></kbd></font> - This will
compile all the standard grains.</p>
<p><fontsize="3"><kbd><strong>compile1grain.in</strong></kbd></font> - example
of compiling a single grain type for the <fontsize="3"><kbd><strong>pgrain</strong></kbd></font>s
<p>The files mewe_fluor.dat and mewe_nelectron.dat are tables 2 and 3 of the atomic data from Kaastra, J.S., & Mewe, R., 1993, A&AS, 97, 443</p>
<p>The file mewe_gbar.dat is the Mewe data files for g-bar collision
strengths.</p>
<hr>
<h2><aname="FeII">FeII</a></h2>
<h3>Data files</h3>
<p>Three files contain the data needed to set up the large FeII model ion,
described in Verner et al. (1999, ApJS 120, 101. The data formats are
described following the name of the file and the reference for the data it
contains.</p>
<h3>fe2rad.dat: </h3>
<p>This file contains Einstein transition probabilities. The original
data sources are given in the header of this file.</p>
<p>lower level number<br>
upper level number<br>
lower level statistical weight<br>
upper level statistical weight<br>
Einstein A coefficient, s**(-1)<br>
Energy, cm**(-1)<br>
type of transition (1 - allowed, 2 - semiforbidden, 3 - forbidden)</p>
<h3>fe2col.dat : </h3>
<p>This file contains collision data. These data are from Zhang &
Pradhan (1995; A&A 293, 953), Bautista (private communication), and the
