Feedback from Active Galactic Nuclei ( AGN ) and subsequent jet cocoons and outflow bubbles can have a significant impact on star formation in the host galaxy .
To investigate feedback physics on small scales , we perform hydrodynamic simulations of realistically fast AGN winds striking Bonnor-Ebert ( BE ) spheres and examine gravitational collapse and ablation .
We test AGN wind velocities ranging from 300–3,000 km s ^ { -1 } and wind densities ranging from 0.5–10 m _ { \mathrm { p } } \mathrm { cm } ^ { -3 } .
We include heating and cooling of low- and high-temperature gas , self-gravity , and spatially correlated perturbations in the shock , with a maximum resolution of 0.01 pc .
We find that the ram pressure is the most important factor that determines the fate of the cloud .
High ram pressure winds increase fragmentation and decrease the star formation rate , but also cause star formation to occur on a much shorter time scale and with increased velocities of the newly formed stars .
We find a threshold ram pressure of \sim 2 \times 10 ^ { -8 } dyne cm ^ { -2 } above which stars are not formed because the resulting clumps have internal velocities large enough to prevent collapse .
Our results indicate that simultaneous positive and negative feedback will be possible in a single galaxy as AGN wind parameters will vary with location within a galaxy .