We report here on the discovery of faint extended wings of H \alpha observed out to an apparent velocity of \sim 7600 km s ^ { -1 } in the Orion Nebula ( M42 ) and in five H II regions in the Large and the Small Magellanic Clouds .
We show that , these wings are caused by Raman scattering of both the O I and Si II resonance lines and stellar continuum UV photons with H I followed by radiative decay to the H I n = 2 level .
The broad wings also seen in H \beta and in H \gamma result from Raman scattering of the UV continuum in the H I n = 4 and n = 5 levels respectively.The Raman scattering fluorescence is correlated with the intensity of the narrow permitted lines of O I and Si II .
In the case of Si II , this is explained by radiative pumping of the same 1023.7Å resonance line involved in the Raman scattering by the Ly \beta radiation field .
The subsequent radiative cascade produces enhanced Si II \lambda \lambda 5978.9 , 6347.1 and 6371.4Å permitted transitions .
Finally we show that in O I , radiative pumping of the 1025.76Å resonance line by the Lyman series radiation field is also the cause of the enhancement in the permitted lines of this species lying near H \alpha in wavelength , but here the process is a little more complex .
We argue that all these processes are active in the zone of the H II region near the ionisation front .