  In order to provide an explanation for the unexpected radial brightness
distribution of the steady accretion discs seen in nova-like variables, Nixon &
Pringle (2019) proposed that the accretion energy is redistributed outwards by
means of strong, magnetically driven, surface flows. In this paper we note that
the "powerful, rotating disc winds" observed in the soft states of black hole
X-ray binaries, and also in the disc around a magnetized neutron star in Her
X-1, have the properties of the outflows postulated by Nixon & Pringle to exist
in the nova-like variable accretion discs around white dwarfs. The relevant
properties are that the flows are not winds, but are, instead, bound flows
(traveling at less than the escape velocity) and that the mass fluxes in the
flows are a substantial fraction of the accretion rate in the disc.
