Core-collapse supernova ( SN ) explosions may occur in the highly inhomogeneous molecular clouds ( MCs ) in which their progenitors were born .
We perform a series of 3-dimensional hydrodynamic simulations to model the interaction between an individual supernova remnant ( SNR ) and a turbulent MC medium , in order to investigate possible observational evidence for the turbulent structure of MCs .
We find that the properties of SNRs are mainly controlled by the mean density of the surrounding medium , while a SNR in a more turbulent medium with higher supersonic turbulent Mach number shows lower interior temperature , lower radial momentum , and dimmer X-ray emission compared to one in a less turbulent medium with the same mean density .
We compare our simulations to observed SNRs , in particular , to W44 , W28 and IC 443 .
We estimate that the mean density of the ambient medium is \sim 10 cm ^ { -3 } for W44 and W28 .
The MC in front of IC 443 has a density of \sim 100 cm ^ { -3 } .
We also predict that the ambient MC of W44 is more turbulent than that of W28 and IC 443 .
The ambient medium of W44 and W28 has significantly lower average density than that of the host giant MC .
This result may be related to the stellar feedback from the SNRs ’ progenitors .
Alternatively , SNe may occur close to the interface between molecular gas and lower density atomic gas .
The region of shocked MC is then relatively small and the breakout into the low density atomic gas comprises most of the SNR volume .