Abstract
Photospheric magnetic elements are most conspicuously visible in high-resolution G-band ltergrams. We show that their enhanced contrast in the G-band is due to a reduction of the CH abundance by dissociation in the deep photospheric layers of the flux tube, where it is hotter than in the surrounding atmosphere. As a consequence, the CH-lines weaken, allowing more of the continuum to \shine through the forest of G-band CH-lines. We suggest that other molecular bands or atomic lines may exhibit a similar behaviour.
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