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There is evidence that the star formation process is linked to the intricatenet of filaments in molecular clouds, which may be also due to gas compressionfrom external triggers. We studied the southern region of the Perseus NGC 1333molecular cloud, known to be heavily shaped by similar external triggers, toshed light on the process that perturbed the filament where the Class 0 IRAS4protostars lie. We use new IRAM-NOEMA observations of SiO and CH3OH, both knownto trace violent events as shocks, toward IRAS 4A as part of the Large ProgramSeeds Of Life in Space (SOLIS). We detected three parallel elongated ($>$6000au) structures, called fingers, with narrow line profiles (~1.5 $km s^{-1}$)peaked at the cloud systemic velocity, tracing gas with high density (5-20$10^5 cm^{-3}$) and high temperature (80-160 K). They are chemically different,with the northern finger traced by both SiO and CH3OH ([CH3OH]/[SiO]~160-300),while the other two only by SiO ([CH3OH]/[SiO]$<$ 40). Among variouspossibilities, a train of three shocks, distanced by $>$5000 yr, would beconsistent with the observations if a substantial fraction of silicon, frozenonto the grain mantles, is released by the shocks.We suggest that the shocktrain is due to an expanding gas bubble, coming behind NGC 1333 from thesouthwest and clashing against the filament, where IRAS 4A lies. Finally, wepropose a solution to the two-decades long debate on the nature and origin ofthe widespread narrow SiO emission observed in the south part of NGC 1333,namely that it is due to unresolved trains of shocks.

A train of shocks at 3000 au scale? Exploring the clash of an expanding bubble into the NGC 1333 IRAS 4 region. SOLIS XIV