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Observational indications of wind-mass transfer from an evolved giant to itsdistant white dwarf (WD) companion in symbiotic binaries are rare. Here, wepresent a way to examine the neutral wind from the giant in symbiotic binaries,which is temporarily observable throughout the orbital plane during outbursts.We find that the mass-loss rate from giants in the orbital plane of S-typesymbiotic binaries is high, indicating a high wind-mass-transfer efficiency inthese systems. We modeled hydrogen column densities in the orbital planebetween the observer and the WD for all suitable eclipsing S-type symbioticbinaries during outbursts in any orbital phase. The mass-loss rate from thegiant in the orbital plane is on the order of 10$^{-6}\,M_{\odot}\,{\rmyr}^{-1}$, which is a factor of $\sim$10 higher than rates derived from nebularemission produced by the ionized wind from normal giants in symbiotic stars.This finding suggests a substantial focusing of the giant's wind toward theorbital plane and, thus, its effective transfer onto the WD companion. Ourfinding suggests that wind focusing on the orbital plane may be a commonproperty of winds from giants in S-type symbiotic stars. Such wind-focusingresolves a long-standing problem of the large energetic output from theirburning WDs and deficient fueling by the giant via a standard Bondi-Hoyleaccretion. It also allows the WD to grow faster in mass, which lends support tothe possibility that S-type symbiotic binaries are progenitors of Type Iasupernovae.

Wind-mass transfer in S-type symbiotic binaries IV. Indication of high wind-mass-transfer efficiency from active phases