5 Conclusions

The results from the analysis of our spectral data of SV Cam could be summarized as follows:

1.

The H$_{\alpha }$ and Fe I 6678 lines have double profiles out of the eclipses. We measured $K_{\rm 1}=123.1$ kms^-1 and $K_{\rm 2}=207.6$ kms^-1 and obtained the mass ratio q=0.593 and masses of the components $M_{\rm 1}=1.47~M_{\odot}$ and $M_{\rm 2}=0.87~M_{\odot}$.

2.

We found the spectral type of the primary component of SV Cam, corresponding to its mass, to be F5V. That is almost one spectral class earlier than previously published. Our spectral type is in good agreement with the color index B-V=0.42, obtained on the basis of our multicolor photometry.

3.

The determined masses and radii of the stellar components of SV Cam obey the mass-radius relation for MS stars.

4.

The measured rotationalal broadenings of the investigated lines correspond to equatorial velocities $V_{\rm eq}^{\rm 1}=116$ kms^-1 and $V_{\rm eq}^{\rm 2}=79$ kms^-1. They agree very well with the values calculated from the obtained radii. Our value of $V_{\rm eq}$ for the primary star is bigger than that (105 kms^-1) measured by Huisong $\&$ Xuefu (1987) and Pojmanski (1998) and close to the value of 117 kms^-1 determined by Hempelmann et al. (1997).

5.

The relatively low S/N ratio of our spectral data does not satisfy the strong requirements of the Doppler imaging technique for surface mapping of stars. We were able to reach only some qualitative conclusions about the surface inhomogeneities of the stellar components and to compare them with the results from the light curve modeling. The analysis of the phase behavior of both H$_{\alpha }$ and FeI 6678 profiles of the primary star showed presence of two cool spots their with maximum visibilities at phases 0.27 and 0.86. In spite of the long time interval between our photometric and spectroscopic observations (more than 2 years), it is surprising that the moving spectral features causing the distortion of the line profiles of the primary star is phase correlated with the visibilities of the two cool spots on its surface.

6.

We found a very good agreement between the global parameters of stars determined from spectroscopic and photometric observations.

7.

The line profiles of SV Cam are considerably deeper at the second quadrature than at the first one. The same behavior of the H$_{\alpha }$ profile of SV Cam was observed recently by Ozeren et al. (2001). The explanation of the absorption established in AB Dor, HK Aqu, SS Boo by cool material in their co-rotating atmospheres (Collier Cameron et al. 1990; Byrne et al. 1996; Hall et al. 1990) is not applicable to our case because the excess absorption for two other short-period RS CVn stars, namely, XY UMa (Kjurkchieva et al. 2000b) and RT And (Kjurkchieva et al. 2001) is visible also around the second quadrature. We have not any explanation for this "quadrature effect" at this time.

As the final result of our investigation, we conclude that there are three activity sources in SV Cam: local active regions (photospheric spots) on the primary star that are observable in photometry as well as in the H$_{\alpha }$ and FeI 6678 lines; enhanced chromospheric emission from the secondary star detectable in the H$_{\alpha }$ line; emission of the circumstellar gas which presence is suspected both in the photometric and spectral data. Probably the three appearances of activity are correlated with each other according to the theory of interacting magnetospheres in RS CVn-type stars (Uchida $\&$ Sakurai 1983).

Acknowledgements

The authors are grateful to the referee for very useful remarks which allowed us to significantly improve this work.