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We use numerical simulations to analyze the evolution and properties ofsuperbubbles (SBs), driven by multiple supernovae (SNe), that propagate intothe two-phase (warm/cold), cloudy interstellar medium (ISM). We consider arange of mean background densities n_avg=0.1-10 cm^{-3} and intervals betweenSNe dt_sn=0.01-1 Myr, and follow each SB until the radius reaches (1-2)H, whereH is the characteristic ISM disk thickness. Except for embedded dense clouds,each SB is hot until a time t_sf,m when the shocked warm gas at the outer frontcools and forms an overdense shell. Subsequently, diffuse gas in the SBinterior remains at T_h 10^6-10^7K with expansion velocity v_h~10^2-10^3km/s(both highest for low dt_sn). At late times, the warm shell gas velocities areseveral 10's to ~100km/s. While shell velocities are too low to escape from amassive galaxy, they are high enough to remove substantial mass from dwarfs.Dense clouds are also accelerated, reaching a few to 10's of km/s. We measurethe mass in hot gas per SN, M_h/N_SN, and the total radial momentum of thebubble per SN, p_b/N_SN. After t_sf,m, M_h/N_SN 10-100M_sun (highest for lown_avg), while p_b/N_SN 0.7-3x10^5M_sun km/s (highest for high dt_sn). Ifgalactic winds in massive galaxies are loaded by the hot gas in SBs, weconclude that the mass-loss rates would generally be lower than star formationrates. Only if the SN cadence is much higher than typical in galactic disks, asmay occur for nuclear starbursts, SBs can break out while hot and expel up to10 times the mass locked up in stars. The momentum injection values, p_b/N_SN,are consistent with requirements to control star formation rates in galaxies atobserved levels.

Superbubbles in the Multiphase ISM and the Loading of Galactic Winds