Contents of: VI/111/./abstract/SGORNY_SKG_ISO.abs

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   From the early days of infrared observations it has been known that
 the planetary nebulae (PNs) have strong dust emission at far-infrared
 wavelengths.  For well observed IRAS sources on the average about 30%
 of the total bolometric flux of PNs comes from the dust component
 which seems to be remnants of the dust shell ejected in the preceding
 asymptotic giant branch phase of evolution. Properties of nebular dust
 are related to the overall chemical evolution during AGB and, in
 particular, could be connected to the phase of nuclear burning at
 which departure from asymptotic giant branch took place. Fig. 1, based
 on the IRAS data, suggests that this can be the case. Figure presents
 locations of planetary nebulae with three different types of central
 stars: Wolf-Rayet type (WR - hydrogen poor, helium burners), other
 emission-lines spectra objects (wels) and hydrogen rich central
 stars (H-rich).

   Therefore it is desirable to study the dust in PNe to understand
 its properties and correlation with central star properties. We
 believe that it would be possible to find out typical characteristics
 of dust which give us an answer about nature of the central star and
 in consequence some information about its preceding evolution. In
 this proposal we seek detailed spectroscopy of the dust emission in
 selected PNe characterized by strong dust emission and with different
 spectral types of central stars. The spectral information which
 the SWS and LWS instruments can provide will for the first time fully
 characterize the dust emission in these PNe (they are not on the GTO
 list). Our radiative transfer and photoionization models should allow
  us to deduce the radial temperature distribution of the dust and
 its chemical composition.

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