  How are accretion discs affected by their outflows? To address this question
for white dwarfs accreting from cool giants, we performed optical, radio,
X-ray, and ultraviolet observations of the outflow-driving symbiotic star MWC
560 (=V694 Mon) during its 2016 optical high state. We tracked multi-wavelength
changes that signalled an abrupt increase in outflow power at the initiation of
a months-long outflow fast state, just as the optical flux peaked: (1) an
abrupt doubling of Balmer absorption velocities; (2) the onset of a $20$
$\mu$Jy/month increase in radio flux; and (3) an order-of-magnitude increase in
soft X-ray flux. Juxtaposing to prior X-ray observations and their coeval
optical spectra, we infer that both high-velocity and low-velocity optical
outflow components must be simultaneously present to yield a large soft X-ray
flux, which may originate in shocks where these fast and slow absorbers
collide. Our optical and ultraviolet spectra indicate that the broad
absorption-line gas was fast, stable, and dense ($\gtrsim10^{6.5}$ cm$^{-3}$)
throughout the 2016 outflow fast state, steadily feeding a lower-density
($\lesssim10^{5.5}$ cm$^{-3}$) region of radio-emitting gas. Persistent optical
and ultraviolet flickering indicate that the accretion disc remained intact.
The stability of these properties in 2016 contrasts to their instability during
MWC 560's 1990 outburst, even though the disc reached a similar accretion rate.
We propose that the self-regulatory effect of a steady fast outflow from the
disc in 2016 prevented a catastrophic ejection of the inner disc. This
behaviour in a symbiotic binary resembles disc/outflow relationships governing
accretion state changes in X-ray binaries.
