We investigate galactic winds driven by supernova ( SN ) explosions in an isolated dwarf galaxy using high-resolution ( particle mass m _ { gas } = 1 { M _ { \odot } } , number of neighbor N _ { ngb } = 100 ) smoothed-particle hydrodynamics simulations that include non-equilibrium cooling and chemistry , individual star formation , stellar feedback and metal enrichment .
Clustered SNe lead to the formation of superbubbles which break out of the disk and vent out hot gas , launching the winds .
We find much weaker winds than what cosmological simulations typically adopt at this mass scale .
At the virial radius , the time-averaged loading factors of mass , momentum and energy are 3 , 1 and 0.05 , respectively , and the metal enrichment factor is 1.5 .
Winds that escape the halo consist of two populations that differ in their launching temperatures .
Hot gas acquires enough kinetic energy to escape when launched while warm gas does not .
However , warm gas can be further accelerated by the ram pressure of the subsequently launched hot gas and eventually escape .
The strong interactions between different temperature phases highlight the caveat of extrapolating properties of warm gas to large distances based on its local conditions ( e.g .
the Bernoulli parameter ) .
Our convergence study finds that wind properties converge when the cooling masses of individual SNe are resolved , which corresponds to m _ { gas } = 5 { M _ { \odot } } with an injection mass of 500 { M _ { \odot } } .
The winds weaken dramatically once the SNe become unresolved .
We demonstrate that injecting the terminal momentum of SNe , a popular sub-grid model in the literature , fails to capture SN winds irrespective of the inclusion of residual thermal energy .