[en] 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 of atomic hydrogen in the wind from the giant. Using our method, we investigated Raman He ii $\mathrm{\lambda <!--\; ??\; -->}1025\to <!--\; ???\; -->\mathrm{\lambda <!--\; ??\; -->}6545$ conversion in the spectrum of the symbiotic Mira V1016 Cyg. We determined its efficiency, η = 0.102, 0.148, and the corresponding mass-loss rate, $\stackrel{\dot{}<!--\; ??\; -->}{M}={2.0}_{-<!--\; ???\; -->0.2}^{+0.1}\times <!--\; ??\; -->{10}^{-<!--\; ???\; -->6},$ ${2.7}_{-<!--\; ???\; -->0.1}^{+0.2}\times <!--\; ??\; -->{10}^{-<!--\; ???\; -->6}$ $M_{\odot <!--\; ???\; -->}{\mathrm{y}\mathrm{r}}^{-<!--\; ???\; -->1}$, using our spectra from 2006 April and 2007 July, respectively. Our values of $\stackrel{\dot{}<!--\; ??\; -->}{M}$ 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.