  Using idealized 1-D Eulerian hydrodynamic simulations, we contrast the
behavior of isolated supernovae with the superbubbles driven by multiple,
collocated supernovae. Continuous energy injection via successive supernovae
going off within the hot/dilute bubble maintains a strong termination shock.
This strong shock keeps the superbubble over-pressured and drives the outer
shock well after it becomes radiative. Isolated supernovae, in contrast, with
no further energy injection, become radiative quite early ($\lesssim 0.1$ Myr,
10s of pc), and stall at scales $\lesssim 100$ pc. We show that isolated
supernovae lose almost all of their mechanical energy by a Myr, but
superbubbles can retain up to $\sim 40\%$ of the input energy in form of
mechanical energy over the lifetime of the star cluster (few 10s of Myr). These
conclusions hold even in the presence of realistic magnetic fields and thermal
conduction. We also compare various recipes for implementing supernova feedback
in numerical simulations. For various feedback prescriptions we derive the
spatial scale below which the energy needs to be deposited for it to couple to
the interstellar medium (ISM). We show that a steady thermal wind within the
superbubble appears only for a large number ($\gtrsim 10^4$) of supernovae. For
smaller clusters we expect multiple internal shocks instead of a smooth, dense
thermalized wind.
