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Context. SuperclusterA in the extragalactic HII region NGC2363 is remarkablefor the hypersonic gas seen as faint extended broad emission lines with a fullwidth zero intensity of 7000km/s. Aims. We explore the possibility that theobserved broad profiles are the result of the interaction of a high velocitycluster wind with dense photoionized clumps. Methods. The geometry consideredis that of near static photoionized condensations at the surface of whichturbulent mixing layers arise as a result of the interaction with the hot wind.The approximative treatment of turbulence is carried out using the mixinglength approach of Canto & Raga. The code mappings Ic is used to derive themean quantities describing the flow and to compute the line emissivities withinthe turbulent layers. The velocity projection in three dimensions of the linesources is carried out analytically. Results. A fast entraining wind of up to~4300km/s appears to be required to reproduce the faint wings of the broadH-alpha and [O III] profiles. A slower wind of 3500km/s, however, can stillreproduce the bulk of the broad component and does provide a better fit than anad hoc Gaussian profile. Conclusions. Radial acceleration in 3D (away fromsupercluster A) of the emission gas provides a reasonable first order fit tothe broad line component. No broad component is predicted for the [N II] and [SII] lines, as observed. The wind velocity required is uncomfortably high andalternative processes that would provide comparable constant acceleration ofthe emission gas up to 4000km/s might have to be considered.

The broad H-alpha, [O III] line wings in stellar supercluster A of NGC2363 and the turbulent mixing layer hypothesis