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We present a comprehensive and self-consistent modelling of the D' typesymbiotic star (SS) HD330036 from radio to UV. Within a colliding-windscenario, we analyse the continuum, line and dust spectra by means of SUMA, acode that simulates the physical conditions of an emitting gaseous cloud underthe coupled effect of ionization from an external radiation source and shocks.We find that the UV lines are emitted from high density gas between the starsdownstream of the reverse shock, while the optical lines are emitted downstreamof the shock propagating outwards the system. As regards with the continuumSED, three shells are identified in the IR, at 850K, 320 K and 200 K with radiir = 2.8 10^13 cm, 4 10^14$ cm, and 10^15 cm, respectively, adopting a distanceto Earth d=2.3 kpc: interestingly, all these shells appear to be circumbinary.The analysis of the unexploited ISO-SWS spectrum reveals that both PAHs andcrystalline silicates coexist in HD330036, with PAHs associated to the internalshell at 850 K, and crystalline silicates stored into the cool shells at 320 Kand 200 K. Strong evidence that crystalline silicates are shaped in a disk-likestructure is derived on the basis of the relative band strengths. Finally, wesuggest that shocks can be a reliable mechanism in activating the annealing andthe consequent crystallization processes. We show that a consistentinterpretation of gas and dust spectra emitted by SS can be obtained by modelswhich accounts for the coupled effect of the photoionizing flux and of shocks.The VLTI/MIDI proposal recently accepted by ESO aims to verify and betterconstrain some of our results by means of IR interferometric observations.

Gas and dust spectra of the D' type symbiotic star HD330036