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New populations of hyper-luminous, dust-obscured quasars have been recentlydiscovered around the peak epoch of galaxy formation ($z \sim 2-3$), inaddition to similar sources found at lower redshifts. Such dusty quasars areoften interpreted as sources `in transition', from dust-enshrouded starburststo unobscured luminous quasars, along the evolutionary sequence. Here weconsider the role of the active galactic nucleus (AGN) radiative feedback,driven by radiation pressure on dust, in high-luminosity, dust-obscuredsources. We analyse how the radiation pressure-driven dusty shell models, withdifferent shell mass configurations, may be applied to the differentpopulations of dusty quasars reported in recent observations. We find thatexpanding shells, sweeping up matter from the surrounding environment, mayaccount for prolonged obscuration in dusty quasars, e.g. for a centralluminosity of $L \sim 10^{47}$erg/s, a typical obscured phase (with extinctionin the range $A_{V} \sim 1-10$ mags) may last a few $\sim 10^6$yr. On the otherhand, fixed-mass shells, coupled with high dust-to-gas ratios, may explain theextreme outflows recently discovered in red quasars at high redshifts. Wediscuss how the interaction between AGN radiative feedback and the ambientmedium at different temporal stages in the evolutionary sequence may contributeto shape the observational appearance of dusty quasar populations.

AGN radiative feedback in dusty quasar populations