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In the present work, we use a photoionisation code to study the H2 emissionof the Helix nebula (NGC 7293) cometary knots, particularly that produced inthe interface H+/H0 of the knot, where a significant fraction of the H2 1-0S(1) emission seems to be produced. Our results show that the production ofmolecular hydrogen in such region may explain several characteristics of theobserved emission, particularly the high excitation temperature of the H2infrared lines.

Modelling H2 Infrared Emission of the Helix Nebula Cometary Knots