The mass-loss rate from Mira variables represents a key parameter in our understanding of their evolutionary tracks . We introduce a method for determining the mass-loss rate from the Mira component in D-type symbiotic binaries via the Raman scattering on atomic hydrogen in the wind from the giant . Using our method , we investigated Raman He II \lambda 1025 \rightarrow \lambda 6545 conversion in the spectrum of the symbiotic Mira V1016 Cyg . We determined its efficiency , \eta = 0.102 , 0.148 , and the corresponding mass-loss rate , \dot { M } = 2.0 ^ { +0.1 } _ { -0.2 } \times 10 ^ { -6 } , 2.7 ^ { +0.2 } _ { -0.1 } \times 10 ^ { -6 } M _ { \odot } { yr } ^ { -1 } , using our spectra from 2006 April and 2007 July , respectively . Our values of \dot { M } that we derived from Raman scattering are comparable with those obtained independently by other methods . Applying the method to other Mira–white dwarf binary systems can provide a necessary constraint in the calculation of asymptotic giant branch ( AGB ) evolution .