4 Discussion

Montes et al. (1995) found that systems with H$_{\alpha }$ emission above the continuum are all cooler than 5000 K. The temperature of the primary star of SV Cam is above this limit and there should be no emission excess expected from it. Our spectral observations show some weak H$_{\alpha }$ emission from the primary star that is connected with its large spots. Rainger et al. (1991) obtained 8 spectra of SV Cam in H$_{\alpha }$ (with S/N=40) that displayed an apparently undisturbed line without any signature of emission.

The analysis of our spectral and photometric data shows that the activity of the primary star is connected with its local surface structures (photospheric spots). Because of the small contribution of the secondary star to the total light (around $10\%$), it is difficult to find evidence for its spots by photometry as well as by spectroscopy. That is why we do not exclude the presence of active regions on the secondary's surface distributed relatively uniformly and close to each other, in contrast to the large spots on the primary star. But the quality of our spectral data allows us to conclude only that the secondary star shows some H$_{\alpha }$ emission excess.

Finally we would like to point out the good agreement between the values for parameters of stars determined by analysis of the spectral data (this paper) and the photometric data (Paper I):

(1) The photometric ratio of the star radii k=0.685 is precisely the same as that determined by the rotational broadenings of their spectral lines k=0.68.

(2) The obtained value of the mass of the primary star corresponds to a F5V star. This value is in good agreement with the color index B-V=0.42 obtained on the basis of our multicolor photometry (Paper I). The mass of the primary star is significantly greater than previously assumed ( $1~M_{\odot}$) based on its adopted spectral type (Budding $\&$ Zeilik 1987; Rainger et al. 1991; Patkos $\&$Hempelmann 1994). The G2-3V classification of Hilditch et al. (1979) was based on photometric observations in the DDO system and in the ubvy Stromgren system and would not give a reliable mass value if the primary star's surface were covered with large cool spots or if there was circumstellar matter present in the system. Our determination of the primary star mass is very close to the value ( $1.42~M_{\odot}$) obtained by Pojmanski (1998) from the near IR spectroscopic observations. We conclude that according to both our photometric and spectroscopic data the spectral types of the SV Cam components are F5 and K4.

(3) It is worth noting that the photometric ratio of the luminosities of the two components in the R band (the range of the two investigated spectral lines) l=0.136 is close to the ratio of the fluxes in the FeI 6678 line (equal to the ratio $EW_{\rm 2}/EW_{\rm 1}$) of 0.143 while the ratio of the fluxes in the H$_{\alpha }$ profiles (0.085) is quite smaller. This fact also confirms the H$_{\alpha }$ emission excess from the secondary star.