Details of the LMC-WNE models

Note: This model grid, put online on 28-Apr-2017, replaces the previous version which, for reference, is still accessible by choosing "LMC-WNE-2013" in the drop-down menu. The major improvement of the new version concerns the iron-group elements. The superlevels are now grouped by states of the same parity. This avoids the spurious emission from Fe III that had been present in the UV spectra of the coolest models in the previous version.

Moreover, ionisation stages of iron (and iron-group elements) up to Fe XVII are now taken into account.

Summary of the model atoms

IonNo. of levels
He I 35
He II 26
He III 1
N I 1
N II 38
N III 85
N IV 38
N V 20
N VI 1
C I 1
C II 32
IonNo. of levels
C III 40
C IV 25
C V 29
C VI 15
G II 1
G III 13
G IV 18
G V 22
G VI 29
G VII 19
IonNo. of levels
G IX 15
G X 28
G XI 26
G XII 13
G XIV 14
G XV 10

Notes: Element "G" stands for the generic iron-group element, which combines the elements from Sc to Ni in solar relative mixture. In case of the "G" element, the number of levels given in the above table actually refers to superlevels.

Contour plots

For a couple of lines, contour plots of the equivalent width have been prepared. The contours are labeled with Wλ in Angstroem:

Hα ps pdf png
Hβ ps pdf png
He I5876 ps pdf png
He II5412 ps pdf png
C IV5801-5812 ps pdf png
N III4640 ps pdf png
N IV4058 ps pdf png
N V4604-4620 ps pdf png
N V4933-4944 ps pdf png

The following contour plot relates the stellar temperature T, which refers to the hydrostatic radius, to the "effective" temperature T2/3 referring to the radius of the optical depth 2/3. The contours are labeled with log T2/3 in Kelvin.

ps pdf png
Original web interface developed by Daniel M. Hamann and Wolf-Rainer Hamann in 2004. PHP-based rework by Andreas Sander (2016).
In case of problems with the PoWR website please contact Wolf-Rainer Hamann (
Astrophysics at the University of Potsdam -- University of Potsdam -- Imprint