5 Conclusion

We present the spectroscopic orbits of eight new subsystems in visual binaries. Of these, only one was known previously, and another one belongs to an optical double star. Remaining 6 systems contribute to the general database on multiple stars with known orbits.

Two systems, ADS 5436 and 11163, have companions with very low masses on 4-day orbits. It was already noted (Tokovinin 1998b) that the periods in the 3 to 6 days range are frequent among multiple stars, much more so than in 6 to 12 days range. The same tendency seems to emerge for the giant planets discovered recently around solar-type stars. It seems natural to suggest that in both cases the orbital evolution was governed by similar processes which first caused orbits to shrink and then froze them at typical periods around 4 days.

Acknowledgements

The author is grateful to the personnel of the Simeis observatory for the possibility to use the 1 m telescope and to M. Mayor who made available CORAVEL. Some measurements were secured by my colleagues N. Gorynya, N. Samus, M. Smekhov, and M. Sachkov. Comments of the referee, T. Mazeh, have served to improve the paper. The database SIMBAD operated at CDS, Strasbourg, France, was consulted. This work was partially supported by the grant from the Russian program "Astronomy''.