tokens: and the microturbulence were related according to Heinzel Anzer (2001) (see Paper I , Appendix A). Therefore, the obvious next step was to use the L and C iii lines to distinguish between kinetic temperature and microturbulence. This is only possible when two species with different masses are formed in the same emitting plasma volume ( Tandberg-Hanssen 1995 ) and are both optically thin. In this section we check whether this condition is met in the spectroscopic UVCS observations of the L, L, and C iii lines. Fig. 2 Doppler velocities of the L, L and C iii lines as a function of latitude along the UVCS slit. Note that the last three points of the L line reach Doppler velocities of several hundred km s. Fig. 3 Profiles of the L, L and C iii lines of the 12th measured point along the erupting prominence. We present a detailed Doppler velocity analysis of all the 68 points we measured along the prominence in the L, L, and C iii lines in Fig. 2 . This shows that for the majority of the points, the Doppler velocities of the C iii line are consistent with the L and L velocities within the uncertainty of the UVCS wavelength determination, which is equal to the spectral UVCS resolution of about 0.2 Å. This gives an uncertainty in the Doppler velocity of about 60 km s. The Doppler velocities of the three lines are almost consistent within the estimated uncertainties. L and L lines must have the same Doppler velocities because they are emitted from the hydrogen atoms. From this we conclude that the C iii ions also move with the same Doppler velocity as hydrogen. Therefore, the L, L and C iii lines are formed in the same or a similar emitting plasma volume with a unique kinetic temperature and microturbulent velocity. In addition, firm proof that all lines are formed in the same plasma volume is provided by the fact that the profiles of all three lines, reported in Fig. 3 in one representative case, exhibit a single peak. We note that their Doppler shifts should be proportional to . If the profiles had more than one peak, it would indicate that the prominence blobs move with different velocities in different directions, and this is not observed. 4. Kinetic temperature and microturbulent velocity The line profiles of optically thin prominences are mainly Doppler broadened as a result of the thermal motions of atoms and because of the turbulent plasma motions. The Doppler line width can then be expressed as Here is the speed of light, is the Boltzmann constant, is the kinetic temperature, is the mass of the atom, is the microturbulent velocity, and is the effective temperature. We introduced the microturbulence because in erupting prominences that are embedded in CME cores, significant nonthermal motions are expected to occur. Equation ( 1 ) shows that the carbon line is more sensitive to the microturbulent velocity and less sensitive to the kinetic temperature, as is clearly shown in Fig. 4 . Fig. 4 Panel a : FWHM of the C iii line plotted as a function
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