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OB type stars have strong ionizing radiation, and drive energetic winds. Theultraviolet (UV) radiation from ionizing stars may heat dust and ionize gas tosweep up an expanding bubble shell. This shell may be the result of feedbackleading to a new generation of stars. N131 is an infrared dust bubble residingin a molecular filament. We study the formation and fragmentation of thisbubble with multi-wavelength dust and gas observations. Towards the bubbleN131, we analyzed archival multi-wavelength observations including 3.6, 4.5,5.8, 8.0, 24, 70, 160, 250, 350, 500 $\mu$m, 1.1 mm, and 21 cm. In addition, weperformed new observations of CO (2-1), CO (1-0), and $^{13}$CO (1-0) with theIRAM 30-m telescope. Multi-wavelength dust and gas observations reveal aringlike shell with compact fragments, two filamentary structures, and asecondary bubble N131-A. The bubble N131 is a rare object with a large hole at24 $\mu$m and 21 cm in the direction of its center. The dust and gas clumps arecompact and might have been compressed at the inner edge of the ringlike shell,while they are extended and might be pre-existing at the outer edge. The columndensity, excitation temperature, and velocity show a potentially hierarchicaldistribution from the inner to outer edge of the ringlike shell. We alsodetected the front and back sides of the secondary bubble N131-A in thedirection of its center. The derived Lyman-continuum ionizing photon fluxwithin N131-A is equivalent to an O9.5 star. Based on the above, we suggestthat the bubble N131 might be triggered by the strong stellar winds from agroup of massive stars inside the bubble. We propose a scenario in which thebubble N131 forms from the disruption of a gas filament by expansion of HIIregion, strong stellar winds, and fragments under self-gravity.

N131: A dust bubble born from the disruption of a gas filament