Two different infrared morphologies within IC 434. In all panels: north is up, east is to the left. Morphology A is evident at every wavelength except for 24 μm, and shows a diffuse structure emanating from the entire L1630 molecular cloud. Morphology B is a relative narrow structure, ranging from the L1630 molecular cloud towards σ Ori AB (white asterisk in the 160 μm images), where it interacts with radiation pressure from the star at projected distance 0.1 <d ≲ 0.4 pc (Paper I), forming the inner dust wave that is visible at wavelengths λ< 24 μm. The 8 μm and 12 μm images show a combination of both morphologies (A+B). The lower panels zoom into the direct surroundings of σ Ori AB and cover the region in the dotted white box seen in the upper panels. The 8 μm, 12 μm and 160 μm images show another arc-like structure at a distance of ~1 pc away from the star (dashed line), forming the outer dust wave. The 12 μm suffer from several ghost features (“G”). The 160 μm image reveals an extended collimated flow (dotted line) away from the σ Ori AB, not seen at 8 μm and 12 μm, which is possibly an evaporating member (“E”) of the large σ Ori cluster. The color bars show the brightness scale in units of MJy/sr.