All Figures

$\begin{figure} \par\includegraphics[angle=270,width=8.7cm,clip]{simultan.eps} \end{figure}$ Figure 1: Timing of IUE (top) and ROSAT (bottom) observations. Time is in JD minus 2 448 900. Note that the orbital frequency of V603 Aql is 7.2 c/d.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=8.8cm,clip]{cross.eps} \end{figure}$ Figure 2: Scan perpendicular to dispersion for a section of a raw spectrum (row m=300). Note the considerable overlap of individualexposures.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{mean1.eps} \end{figure}$ Figure 3: Statistical properties of UV spectra: standard deviation per single spectrum (a, shifted by -12) and average spectrum (b), both in log Flux units, where flux is in $\mbox{(erg~ cm}^{-2}~\mbox{s}^{-1}~\mbox{\AA}^{-1}\mbox{)}$ . Letters (G) and (R) mark structures affected respectively by the geocoronal radiation and reseau mark.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=8.8cm,clip]{lightcurve.eps} \end{figure}$ Figure 4: Continuum (wavelength band 1575-1625 Å) and CIV1550 emission line lightcurves. The continuum points are denoted by black diamonds and the CIV1550 points by open circles. The time is in JD minus 2 448 900.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=8.8cm,clip]{old.eps} \end{figure}$ Figure 5: Same as Fig. 4 for observations from 1989 except that the horizontal axis id JD minus 2 447 689. Note that the scatter of observations is one third that observed in 1992 with the same instrument setup and reduction techniques.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=8.8cm,clip]{freq-rosat-wide.eps} \end{figure}$ Figure 6: Power spectrum for the integrated X-ray lightcurve in 400 s bins. On the horizontal axis is frequency in cycles per day.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=8.8cm,clip]{freq-lines.eps} \end{figure}$ Figure 7: Power spectrum for the CIV1550 Å emission line.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=8.8cm,clip]{korel-cont-cont.eps} \end{figure}$ Figure 8: Autocorrelation function for UV continuum. On the horizontal axis is the time lag in days.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=8.8cm,clip]{korel-x-x.eps} \end{figure}$ Figure 9: Autocorrelation function for X-ray. Scales as in Fig. 8.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=8.8cm,clip]{korel-lines-lines.eps} \end{figure}$ Figure 10: Autocorrelation function for CIV1550 Å emission line (vertical axis). Scales as in Fig. 8. Note that the maxima repeat with the orbital period.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=8.8cm,clip]{l-x.eps} \end{figure}$ Figure 11: Cross-correlation function (CCF) for CIV1550 emission vs. X-ray integrated flux (vertical axis). Horizontal axis is time lag in days. The lag is positive when X-ray variations trail behind CIV1550. Note a periodic structure related to orbital modulation of CIV1550 (see text).
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=8.8cm,clip]{color-x.eps} \end{figure}$ Figure 12: The same as in Fig. 11 for UV color vs. X-ray integrated flux. Note the feature at the lag +0.11 d discussed in Sect. 4.3.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{X-UV1.eps} \end{figure}$ Figure 13: UV continuum against X-ray flux at zero lag (< $0.00501~\mbox{d}$ ). X-units: PSPC counts per 400 s time bin, y-units: $\mbox{erg~ cm}^{-2}~\mbox{s}^{-1}~\mbox{\AA}^{-1}/\mbox{30}$ . Note that clustering around the diagonal indicates a positive correlation. According to Student t-test (Fisz 1963) the correlation is significant at the level P=0.0001, corresponding to $3.9\sigma$ .
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=8.8cm,clip]{averspec.eps} \end{figure}$ Figure 14: Average profile of CIV1550 Å line, from 100 IUE spectra. On horizontal axis wavelength in Å. Error bars indicate $\pm$ $\sigma$ range of the mean. The scatter of the individual spectra is 10 times more.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=16.5cm,clip]{4x1a.eps} \end{figure}$ Figure 15: CIV1550 line, at phases $\phi _{\rm em}=0.550, 0.568, 0.633, 0.646$ . Scales as in Fig. 14.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=8.8cm,clip]{absorbcja.eps} \end{figure}$ Figure 16: Power spectrum of strength of the absorption component of CIV1550 line. X axis is frequency in cycles per day.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=8.8cm,clip]{faza_CIV.eps} \end{figure}$ Figure 17: Intensity of CIV1550 emission line phase, in $\mbox{erg~ cm}^{-2}~\mbox{s}^{-1}~\mbox{\AA}^{-1}$ , folded and binned with the orbital period. Phase 0 corresponds to $\mbox{HJD 2448903.1397}$ . To explain this modulation at orbital inclination $i\sim 20$ we postulate absorption by an asymmetric wind.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=8.8cm,clip]{SiIVmean.eps} \end{figure}$ Figure 18: Average profile of SiIV1393/1402 Å doublet line, from 100 IUE spectra. Error bars indicate $\pm 1\sigma$ range of the mean. Scatter of individual observations is 10 times more.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=8.8cm,clip]{siIV.eps} \end{figure}$ Figure 19: Power spectrum of intensity of the SiIV1393/1402 Å doublet emission line.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=8.7cm,clip]{simultan.eps} \end{figure}$	Figure 1: Timing of IUE (top) and ROSAT (bottom) observations. Time is in JD minus 2 448 900. Note that the orbital frequency of V603 Aql is 7.2 c/d.
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$\begin{figure} \par\includegraphics[angle=270,width=8.8cm,clip]{cross.eps} \end{figure}$	Figure 2: Scan perpendicular to dispersion for a section of a raw spectrum (row m=300). Note the considerable overlap of individualexposures.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{mean1.eps} \end{figure}$	Figure 3: Statistical properties of UV spectra: standard deviation per single spectrum (a, shifted by -12) and average spectrum (b), both in log Flux units, where flux is in $\mbox{(erg~ cm}^{-2}~\mbox{s}^{-1}~\mbox{\AA}^{-1}\mbox{)}$ . Letters (G) and (R) mark structures affected respectively by the geocoronal radiation and reseau mark.
Open with DEXTER

$\begin{figure} \par\includegraphics[angle=270,width=8.8cm,clip]{lightcurve.eps} \end{figure}$	Figure 4: Continuum (wavelength band 1575-1625 Å) and CIV1550 emission line lightcurves. The continuum points are denoted by black diamonds and the CIV1550 points by open circles. The time is in JD minus 2 448 900.
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$\begin{figure} \par\includegraphics[angle=270,width=8.8cm,clip]{old.eps} \end{figure}$	Figure 5: Same as Fig. 4 for observations from 1989 except that the horizontal axis id JD minus 2 447 689. Note that the scatter of observations is one third that observed in 1992 with the same instrument setup and reduction techniques.
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$\begin{figure} \par\includegraphics[angle=270,width=8.8cm,clip]{freq-rosat-wide.eps} \end{figure}$	Figure 6: Power spectrum for the integrated X-ray lightcurve in 400 s bins. On the horizontal axis is frequency in cycles per day.
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$\begin{figure} \par\includegraphics[angle=270,width=8.8cm,clip]{freq-lines.eps} \end{figure}$	Figure 7: Power spectrum for the CIV1550 Å emission line.
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$\begin{figure} \par\includegraphics[angle=270,width=8.8cm,clip]{korel-cont-cont.eps} \end{figure}$	Figure 8: Autocorrelation function for UV continuum. On the horizontal axis is the time lag in days.
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$\begin{figure} \par\includegraphics[angle=270,width=8.8cm,clip]{korel-x-x.eps} \end{figure}$	Figure 9: Autocorrelation function for X-ray. Scales as in Fig. 8.
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$\begin{figure} \par\includegraphics[angle=270,width=8.8cm,clip]{korel-lines-lines.eps} \end{figure}$	Figure 10: Autocorrelation function for CIV1550 Å emission line (vertical axis). Scales as in Fig. 8. Note that the maxima repeat with the orbital period.
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$\begin{figure} \par\includegraphics[angle=270,width=8.8cm,clip]{l-x.eps} \end{figure}$	Figure 11: Cross-correlation function (CCF) for CIV1550 emission vs. X-ray integrated flux (vertical axis). Horizontal axis is time lag in days. The lag is positive when X-ray variations trail behind CIV1550. Note a periodic structure related to orbital modulation of CIV1550 (see text).
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$\begin{figure} \par\includegraphics[angle=270,width=8.8cm,clip]{color-x.eps} \end{figure}$	Figure 12: The same as in Fig. 11 for UV color vs. X-ray integrated flux. Note the feature at the lag +0.11 d discussed in Sect. 4.3.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{X-UV1.eps} \end{figure}$	Figure 13: UV continuum against X-ray flux at zero lag (< $0.00501~\mbox{d}$ ). X-units: PSPC counts per 400 s time bin, y-units: $\mbox{erg~ cm}^{-2}~\mbox{s}^{-1}~\mbox{\AA}^{-1}/\mbox{30}$ . Note that clustering around the diagonal indicates a positive correlation. According to Student t-test (Fisz 1963) the correlation is significant at the level P=0.0001, corresponding to $3.9\sigma$ .
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$\begin{figure} \par\includegraphics[angle=270,width=8.8cm,clip]{averspec.eps} \end{figure}$	Figure 14: Average profile of CIV1550 Å line, from 100 IUE spectra. On horizontal axis wavelength in Å. Error bars indicate $\pm$ $\sigma$ range of the mean. The scatter of the individual spectra is 10 times more.
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$\begin{figure} \par\includegraphics[angle=270,width=16.5cm,clip]{4x1a.eps} \end{figure}$	Figure 15: CIV1550 line, at phases $\phi _{\rm em}=0.550, 0.568, 0.633, 0.646$ . Scales as in Fig. 14.
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$\begin{figure} \par\includegraphics[angle=270,width=8.8cm,clip]{absorbcja.eps} \end{figure}$	Figure 16: Power spectrum of strength of the absorption component of CIV1550 line. X axis is frequency in cycles per day.
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$\begin{figure} \par\includegraphics[angle=270,width=8.8cm,clip]{faza_CIV.eps} \end{figure}$	Figure 17: Intensity of CIV1550 emission line phase, in $\mbox{erg~ cm}^{-2}~\mbox{s}^{-1}~\mbox{\AA}^{-1}$ , folded and binned with the orbital period. Phase 0 corresponds to $\mbox{HJD 2448903.1397}$ . To explain this modulation at orbital inclination $i\sim 20$ we postulate absorption by an asymmetric wind.
Open with DEXTER

$\begin{figure} \par\includegraphics[angle=270,width=8.8cm,clip]{SiIVmean.eps} \end{figure}$	Figure 18: Average profile of SiIV1393/1402 Å doublet line, from 100 IUE spectra. Error bars indicate $\pm 1\sigma$ range of the mean. Scatter of individual observations is 10 times more.
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$\begin{figure} \par\includegraphics[angle=270,width=8.8cm,clip]{siIV.eps} \end{figure}$	Figure 19: Power spectrum of intensity of the SiIV1393/1402 Å doublet emission line.
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