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UV observations with IUE have led to recognition of the importance of di-electronic recombination in PN, for the calculation of ionization equilibria and for production of the features C II X1335 and C III X2297. The determination of C abundances is discussed. In high-excitation nebulae one must allow for absorption of C IV X154-9 by dust. It has been shown that C/0 < 0.5 for five PN with a silicate IR feature and that C/0 > 1 for four with a SiC feature. Dust opacities T n have been deduceddoi:10.1007/978-94-009-7094-6_15 fatcat:3dgeg3hmuvbtfgu23pkc64qple