The theoretical Stark HWHM dependence on the electron temperature together
with the values of the other authors and our experimental results at the
electron density of
m-3 are presented graphically in Figs. 3 (click here), 4 (click here)
and 5 (click here), assuming the domination of the electron impact mechanism to the line
broadening, for the investigated NII, NIII and NIV spectral lines,
respectively.
Figure 3: Theoretical Stark HWHM dependence on the electron
temperature scaled to the electron density of 
m-3
for the NII spectral lines. 
our experimental results and those of the
other authors: 
Berg et al. (1967);
Konjevic et al. (1970);
Jalufka & Craig (1975);
Popovic et al. (1975); 
Källne et al. (1979);
Purcell & Barnard (1984)
and 
Djenize et al. (1992). SC, G and GM denote values obtained on
the basis of the semiclassical (Griem 1974) approximation, but SEM and SE
denote values obtained on the basis of the modified semiempirical and
semiempirical approximations, respectively. All these calculations were
performed by Dimitrijevic & Konjevic (1980, 1981a,b). 
is the mean
wavelength for the multiplet. The error bars include the uncertainties of the
width and electron density measurements
Figure 4: Theoretical Stark HWHM dependence on the electron
temperature scaled to the electron density of m-3
for the NIII
spectral lines. The symbols are the same as in Fig. 3 (click here);
in addition
,
Puric et al. (1987) and *,
Glenzer et al. (1994)
at approximately 100 000 K electron temperature
Figure 5: Theoretical Stark HWHM dependence on the electron
temperature scaled to the electron density of m-3
for the NIV spectral lines. The symbols are the same as in Fig. 3 (click here); in addition
, Puric et al. (1987)
On the basis of the 
values from the Table 1 (click here)
and Figs. 3 (click here), 4 (click here) and 5 (click here) we can conclude that in the cases of the investigated NII and NIII
spectral lines our experimental Stark HWHM values well agree, within the
experimental accuracy and the reliability of theory, with the value calculated
on the basis of the modified semiempirical (SEM) approximation. For the NIV
spectral lines this statement can be applied, also, but for the theoretical
values calculated on the basis of the semiclassical (G) approximation. It
should be pointed out that the Stark HWHM data measured by
Glenzer et al. (1994)
(at approximately 100 000 K electron temperature and
m-3
electron
density it is 0.0093 nm) and Puric et al. (1987) shows,
for the multiplet No. 3
in NIII spectra, agreement with the predictions based on the SEM approximation,
within the experimental accuracy.
No calculated Stark HWHM values exist for the spectral lines, at electron temperatures higher than 40 000 K, from the multiplets Nos. 3, 5 and 28 in NII spectra, Nos. 8, 13 and UV25 in NIII spectra and No. 8 in NIV spectra, to the knowledge of the authors. Therefore, the comparison of our Stark HWHM data of relevant spectral lines with theory is omitted.
In the case of the Stark shifts the situation is different.
Namely, the measured values 
, normalized to an
m-3 electron density,
are generally very small, within experimental error 
0.0015 nm)
they are close
to zero. Early measurements of the Stark shift values for the NIII spectral
lines (Puric et al. 1988) and for the NII
spectral lines (Djenize et al. 1992)
referee, also, very small Stark shift values. No calculated Stark shift values
exist for the investigated NIV spectral lines, therefore, the comparison there
with our measured values is omitted.