Details of the re-calculated WNE models (2013)

The major improvement over the 2004 version of the models concerns the model atoms, which have been extended in order to achieve a more complete coverage of the near-IR J, H and K bands.

Note: This model grid originally suffered from a bug in the atomic data, which affected a few spectral lines. Especially the N_V multiplett at 4933-4944 became far too strong by this bug. The grid was replaced by a corrected version on 2013 November 4.

Summary of the model atoms:

IonNo. of levels
He I 35
He II 26
He III 1
N II 1
N III 36
N IV 38
N V 20
IonNo. of levels
N VI 1
C II 3
C III 40
C IV 21
C V 1
G II 1
G III 8
IonNo. of levels
G IV 11
G V 13
G VI 17
G VII 11
G VIII 9
G IX 9
G X 1

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.

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

H α ps pdf png
H β ps pdf png
He I 5876 ps pdf png
He II 5412 ps pdf png
N III 4640 ps pdf png
N IV 4058 ps pdf png
N V 4604-4620 ps pdf png
N V 4933-4944 ps pdf png
C IV 5801-5812 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
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