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Considering the physical conditions that are relevant for triggering starformation in interactions involving SN shocks and neutral clouds, we have builtdiagrams of the SNR radius versus the cloud density in which these conditionsconstrain a shaded zone where star formation is allowed. The diagrams are alsotested with fully 3-D MHD radiative cooling simulations involving a SNR and aself-gravitating cloud and we find that the numerical analysis is consistentwith the results predicted by the diagrams. While the inclusion of ahomogeneous magnetic field approximately perpendicular to the impact velocityof the SNR with an intensity ~1 $mu$G results only a small shrinking of thestar formation zone in the diagrams, a larger magnetic field (~10 $\mu$G)causes a significant shrinking, as expected. Applications of our results toreal star formation regions in our own galaxy have revealed that theirformation could have been triggered by a SN shock wave. Finally, we haveevaluated the effective global star formation efficiency of this sort ofinteractions and found that it is smaller than the observed values in ourGalaxy (SFE ~0.01-0.3). This result is consistent with previous work in theliterature and also suggests that the mechanism presently investigated, thoughvery powerful to drive structure formation, supersonic turbulence andeventually, local star formation, does not seem to be sufficient to driveglobal star formation in normal star forming galaxies.

Star formation triggered by SNR impact into magnetized neutral clouds