Mass-loss Rate by the Mira in the Symbiotic Binary V1016 Cygni from Raman Scattering

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 λ 1025\to λ 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, \dot{M}={2.0}_-0.2^+0.1× {10}^-6, {2.7}_-0.1^+0.2× {10}^-6 {M}_⊙ {{{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.