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We perform two dimensional hydrodynamic numerical simulations to study thepositive active galactic nucleus feedback which triggers, rather thansuppresses, star formation. Recently, it was shown by Nayakshin et al. andIshibashi et al. that star formation occurs when the cold interstellar mediumis squeezed by the impact of mass outflow or radiation pressure, respectively.Mass outflow is ubiquitous in this astrophysical context, and radiationpressure is also important if the AGN is luminous. For the first time in thissubject, we incorporate both mass outflow feedback and radiative feedback intoour model. Consequently, the ISM is shocked into shells by the AGN feedback,and these shells soon fragment into clumps and filaments because ofRayleigh-Taylor and thermal instabilities. We have two major findings: (1) thestar formation rate can indeed be very large in the clumps and filaments.However, the resultant star formation rate density is too large compared withprevious works, which is mainly because we ignore the fact that most of thestars that are formed would be disrupted when they move away from the galacticcenter. (2) Although radiation pressure feedback has a limited effect, whenmass outflow feedback is also included, they reinforce each other.Specifically, in the gas-poor case, mass outflow is always the dominantcontributor to feedback.

Triggering star formation by both radiative and mechanical active galactic nucleus feedback