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A spectrum from 8-13 $\mu$m of the FU Ori star V1057 Cyg was obtained on 23 Jun 1992 UT with the CGS3 instrument at the United Kingdom Infrared Telescope on Mauna Kea. A double peaked silicate emission feature is evident. Assuming optically thin emission, the emissivity of the silicate grains is estimated. The first peak is not well-defined, but occurs between 9.6-10.1 $\mu$m; the second occurs at $\sim11.2$ $\mu$m. The feature profile does not resemble that commonly seen in molecular clouds (the ``Trapezium'' profile). It does resemble the silicate feature seen in comet Halley and certain other comets. Similar features are seen around the young stellar object Elias 1 and around $\beta$ Pic (Knacke et al. 1992, BAAS, 24, 789). In these objects, the 11.2 $\mu$m feature has been attributed to crystalline olivine. Whatever mechanism has served to anneal some of the silicates in comets may occur during the early stages of a star's life.
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