Double-Peaked Silicate Emission in the FU Ori Star V1057 Cyg
Session 62 -- Very Young Stars
Display presentation, Thursday, 9:20-4:00, Pauley Room

## [62.23] Double-Peaked Silicate Emission in the FU Ori Star V1057 Cyg

T.Y. Brooke (JPL/Caltech), M.S. Hanner (JPL/Caltech), A.T. Tokunaga (IfA/U. Hawaii)

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.