Double-Peaked Silicate Emission in the FU ORI Star V1057 CYG

Details Double-Peaked Silicate Emission in the FU ORI Star V1057 CYG Double-Peaked Silicate Emission in the FU ORI Star V1057 CYG

May 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993aas...182.6223b&link_type=abstract

American Astronomical Society, 182nd AAS Meeting, #62.23; Bulletin of the American Astronomical Society, Vol. 25, p.907

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Scientific paper

A spectrum from 8-13 microns 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 microns; the second occurs at ~ 11.2 microns. 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 microns 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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