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In this paper we study new infrared spectra of the evolved planetary nebulaNGC 6445 obtained with ISO. These data show that the thermal emission from thegrains is very cool and has a low flux compared to H beta. A model of theionized region is constructed, using the photo-ionization code CLOUDY 90.05.Based on this model, we show from depletions in the gas phase elements thatlittle grain destruction can have occurred in the ionized region of NGC 6445.We also argue that dust-gas separation in the nebula is not plausible. The mostlikely conclusion is that grains are residing inside the ionized region of NGC6445 and that the low temperature and flux of the grain emission are caused bythe low luminosity of the central star and the low optical depth of the grains.This implies that the bulk of the silicon-bearing grains in this nebula wereable to survive exposure to hard UV photons for at least several thousands ofyears, contradicting previously published results.  A comparison between optical and infrared diagnostic line ratios gives amarginal indication for the presence of a t^2-effect in the nebula. However,the evidence is not convincing and other explanations for the discrepancy arealso plausible.  The off-source spectrum taken with ISO-LWS clearly shows the presence of awarm cirrus component with a temperature of 24 K as well as a very coldcomponent with a temperature of 7 K. Since our observation encompasses only asmall region of the sky, it is not clear how extended the 7 K component is andwhether it contributed significantly to the FIRAS spectrum taken by COBE.Because our line of sight is in the galactic plane, the very cold componentcould be a starless core.Comment: 36 pages, 8 tables, 7 figures, accepted for publication in Ap

Properties of Dust Grains in Planetary Nebulae. I. The Ionized Region of NGC 6445