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We report the results of spectroscopic observations and numerical modellingof the H II region IRAS 18153-1651. Our study was motivated by the discovery ofan optical arc and two main-sequence stars of spectral type B1 and B3 near thecentre of IRAS 18153-1651. We interpret the arc as the edge of the wind bubble(blown by the B1 star), whose brightness is enhanced by the interaction with aphotoevaporation flow from a nearby molecular cloud. This interpretationimplies that we deal with a unique case of a young massive star (the mostmassive member of a recently formed low-mass star cluster) caught just tens ofthousands of years after its stellar wind has begun to blow a bubble into thesurrounding dense medium. Our two-dimensional, radiation-hydrodynamicssimulations of the wind bubble and the H II region around the B1 star provide areasonable match to observations, both in terms of morphology and absolutebrightness of the optical and mid-infrared emission, and verify the young ageof IRAS 18153-1651. Taken together our results strongly suggest that we haverevealed the first example of a wind bubble blown by a main-sequence B star.

IRAS 18153-1651: an H II region with a possible wind bubble blown by a young main-sequence B star