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Massive stars inject mechanical and radiative energy into the surroundingenvironment, which stirs it up, heats the gas, produces cloud and intercloudphases in the interstellar medium, and disrupts molecular clouds (the birthsites of new stars). Stellar winds, supernova explosions and ionization byultraviolet photons control the lifetimes of molecular clouds. Theoreticalstudies predict that momentum injection by radiation should dominate that bystellar winds, but this has been difficult to assess observationally.Velocity-resolved large-scale images in the fine-structure line of ionizedcarbon ([C II]) provide an observational diagnostic for the radiative energyinput and the dynamics of the interstellar medium around massive stars. Here wereport observations of a one-square-degree region (about 7 parsecs in diameter)of Orion molecular core -- the region nearest to Earth that exhibitsmassive-star formation -- at a resolution of 16 arcseconds (0.03 parsecs) inthe [C II] line at 1.9 terahertz (158 micrometres). The results reveal that thestellar wind originating from the massive star ${\theta}^{1}$ Orionis C hasswept up the surrounding material to create a bubble roughly four parsecs indiameter with a 2,600-solar-mass shell, which is expanding at 13 kilometres persecond. This finding demonstrates that the mechanical energy from the stellarwind is converted very efficiently into kinetic energy of the shell and causesmore disruption of the Orion molecular core 1 than do photo-ionization andevaporation or future supernova explosions.

Disruption of the Orion Molecular Core 1 by the stellar wind of the massive star ${\theta}^1$ Ori C