Each Tarball contains subdirectories for every grid model.
In each subdirectory, the file "flux_calib.dat"
contains an xy-table with
wavelengths and absolute flux (models have log L/L☉ = 5.3),
whereas the file "flux.pdf" contains a log-log diagram of the SED for
quick inspection. Please refer to the PoWR homepage
for detailed information about these grids.
Please, don't forget to cite the corresponding papers:
Galactic WN grids,
LMC WN grids
SMC grids: Hainich et al. (2015)
WN grids in general: Todt et al. (2015)
Line-blanketed model atmospheres for WR stars
A temperature correction method for expanding atmospheres
Grids of model spectra for WN stars, ready for use
Range is 200 - 80000 Å, resolution is 0.3 vDopp = 30
km/s, models include now improved iron files (parity splitting)
For models with Rt ≤ 0.4 Rsun (so
Rt index ≥ 17, see Fig.) there is a
degeneracy. That means that the spectra of models along "diagonal"
in the model grid look the same.
Models along these diagonals have the same mass-loss rate Mdot; and
T* and Rt are not longer good parameters, but
instead L* and Mdot. So, if you miss e.g. model 16-20 you
can instead also use 15-19.
Model grid for Galactic WC stars with some fit results. Note the
area of parameter degeneracy: models along the shown diagonal lines
have same emergent spectrum (see above). This can also be seen in the
contour plots for spectral lines and Tτ=2/3
contour plot for WNE grid
- Spikes in the far Infrared spectrum (above 20 μm):
Some lines, e.g. He II 9 - 8 (69477.11 Ang in WO20-25v2000)
or C IV 4d J5/2- 4p J3/2 (49592.11 Ang in WC20-25) tend to schow Laser
features, i.e. spikes in the line profiles. In this examined
example (WO 20-25 v2000), the He II 9-8 line has a spike 100x above
continuum at about -v∞.
- Ionizing fluxes: usually one should use the numbers obtained
from coli program (as given on the PoWR website). However, even
these values must be considered carefully, especially for numbers
below log Q < 44.0 (optically thick models at outer boundaries). These
values are most often in fact 0.0 (dex), especially for cooler
models and for He II ionizing photons. After the 2015 update of the
iron data (parity splitting) the values of most log Q (H I) for
cooler models have increased by a factor of 2 or 3.