Table 1: The components of the lithium-like Mg  X doublet and the emission lines in their neighbourhoods.
Lines Wavelengtha Radiances Remarks
  $\lambda$/nm $L_{\rm K}^{b}$ $L_{\rm C}^{c}$  
O  IV   60.8398 800 731 outside Fig. 2
O  V 121.834 - -  
O  III   60.9705 300 1.61 blend
Mg  X   60.9795 23 457 blend
O  IV   60.9829 850 1300 blendd
O  III   61.0043 350 5.26 not visible
C  I 124.9004 10 -  
O  IV   62.4617 750 3.27  
Si  X   62.470 - -  
C  I 124.9405 20 -  
P  II 124.9812 - - blend
Mg  X   62.4965 12 227 blend
Mg  II 124.993 - - blend
Si  II 125.0089 100 - blend
O  IV   62.5130 800 6.57 blend
C  I 125.0423 30 -  
Si  II 125.0433 150 -  
S  II 125.0578 - - prominent
Si  II 125.1164 200 - weak
C  I 125.1176 40 -  
O  IV   62.5852 850 9.82 weak
a For line identifications and wavelengths see Cohen et al. (1978); Sandlin et al. (1986); Kelly (1987); Dammasch et al. (1999); Peter & Judge (1999), and Curdt et al. (2001). The first and second orders of diffraction are superimposed in SUMER spectra.
b Relative radiances after Kelly (1987); separately given for the different spectra listed with more than one line.
c Relative radiances derived from CHIANTI (cf. Dere et al. 1997) for isothermal plasmas at the formation temperature of each line and a density of $n_{\rm e} = 1 \times 10^9~{\rm cm}^{-3}$.
d Relative radiance of O  IV is 15% of L(Mg  X) + L(O  IV) at 29 $^{\prime \prime }$ to 80 $^{\prime \prime }$ above the limb.

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