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Stellar feedback from high-mass stars (e.g., H{\sc ii} regions) can stronglyinfluence the surrounding interstellar medium and regulate star formation. Ournew ALMA observations reveal sequential high-mass star formation taking placewithin one sub-virial filamentary clump (the G9.62 clump) in the G9.62+0.19complex. The 12 dense cores (MM 1-12) detected by ALMA are at very differentevolutionary stages, from starless core phase to UC H{\sc ii} region phase.Three dense cores (MM6, MM7/G, MM8/F) are associated with outflows. Themass-velocity diagrams of outflows associated with MM7/G and MM8/F can be wellfitted with broken power laws. The mass-velocity diagram of SiO outflowassociated with MM8/F breaks much earlier than other outflow tracers (e.g., CO,SO, CS, HCN), suggesting that SiO traces newly shocked gas, while the othermolecular lines (e.g., CO, SO, CS, HCN) mainly trace the ambient gascontinuously entrained by outflow jets. Five cores (MM1, MM3, MM5, MM9, MM10)are massive starless core candidates whose masses are estimated to be largerthan 25 M$_{\sun}$, assuming a dust temperature of $\leq$ 20 K. The shocks fromthe expanding H{\sc ii} regions ("B" \& "C") to the west may have great impacton the G9.62 clump through compressing it into a filament and inducing corecollapse successively, leading to sequential star formation. Our findingssuggest that stellar feedback from H{\sc ii} regions may enhance the starformation efficiency and suppress the low-mass star formation in adjacentpre-existing massive clumps.

ALMA reveals sequential high-mass star formation in the G9.62+0.19 complex