  Galactic outflows from local starburst galaxies typically exhibit a layered
geometry, with cool $10^4\,$K flow sheathing a hotter $10^7\,$K,
cylindrically-collimated, X-ray emitting plasma. Here, we argue that winds
driven by energy-injection in a ring-like geometry can produce this distinctive
large-scale multi-phase morphology. The ring configuration is motivated by the
observation that massive young star clusters are often distributed in a ring at
the host galaxy's inner Lindblad resonance, where larger-scale spiral arm
structure terminates. We present parameterized three-dimensional radiative
hydrodynamical simulations that follow the emergence and dynamics of
energy-driven hot winds from starburst rings. In this Letter, we show that the
flow shocks on itself within the inner ring hole, maintaining high $10^7$\,K
temperatures, whilst flows that emerge from the wind-driving ring unobstructed
can undergo rapid bulk cooling down to $10^4\,$K, producing a fast hot
bi-conical outflow enclosed by a sheath of cooler nearly co-moving material
without ram-pressure acceleration. The hot flow is collimated along the ring
axis, even in the absence of pressure confinement from a galactic disk or
magnetic fields. In the early stages of expansion, the emerging wind forms a
bubble-like shape reminiscent of the Milky Way's eROSITA and Fermi bubbles and
can reach velocities usually associated with AGN-driven winds. We discuss the
physics of the ring configuration, the conditions for radiative bulk cooling,
and the implications for future X-ray observations.
