Abstract
We present a new model to explain the excess in mid and near infrared emission of V605 Aql. This hydrogen poor object is of special interest because it formed after a late helium flash of the central star in the planetary nebula Abell 58. Simple grain size models with an equilibrium dust temperature cannot explain ISO and IRAS measurements. Environmental condition and grain parameters are discussed to extend standard models with temperature fluctuations and a grain size distribution.
