RADIAL-VELOCITIES OF THE SYMBIOTIC NOVA HM SAGITTAE

The radial velocities of the symbiotic nova HM Sge have been determine d from the spectrograms obtained in 1984-1995 with the UAGS spectrogra ph attached to the 125-cm telescope of the Crimean Station of the Ster nberg Astronomical Institute. The radial-velocity variations were foun d to correlate with the pulsation phase of the Mira variable in the sy stem HM Sge with a period of 527(d) (Munari and Whitelock 1989). These results lend support to the hypothesis that the emission Lines in HM Sge are formed at the interface of the winds from the cool and hot com ponents. A summary of radial-velocity measurements of HM Sge collected from published data is given.