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Time resolved spectroscopy of the pulsating CV GW Lib

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Figure

Table 1. Observations of GW Lib
Figure 1 shows the ew evolution for the Balmer lines andthe middle panel the same for the helium lines
Figure 3. Normalised emission line profiles of Hare the various Gaussian profiles fits and theHedoublet has, most likely, a very similar origin as the Hcases the average profile over 1 orbital period
Table 2. Equivalent widths in in a˚A ±3σ error, of various emission lines as function of the outburst
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