Spectrophotometry of OH 26.5+0.6 from 2 to 40 microns

Details Spectrophotometry of OH 26.5+0.6 from 2 to 40 microns Spectrophotometry of OH 26.5+0.6 from 2 to 40 microns

Jan 1978

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978apj...219..114f&link_type=abstract

Astrophysical Journal, Part 1, vol. 219, Jan. 1, 1978, p. 114-120.

Astronomy and Astrophysics

Astronomy

81

Black Body Radiation, Infrared Astronomy, Late Stars, Spectral Energy Distribution, Stellar Envelopes, Stellar Spectrophotometry, Variable Stars, Absorption Spectra, Cosmic Dust, Radio Attenuation, Stellar Mass Ejection

Scientific paper

Airborne and ground-based observations show that OH 26.5+0.6 has strong 10 micrometers and weak 18 micrometers silicate absorptions superposed on an overall energy distribution much like a blackbody. The flux level, color temperature, and depth of the 10 micrometers absorption have varied during two years of observations. A model of the source as a late-type variable star that has ejected an optically thick dust shell is suggested; the mass-loss rate implied is greater than about 0.00001 solar masses per year. The fact that significant flux from the source is observed between 4 and 7 micrometers is evidence that oxygen-rich dust has significant opacity in that wavelength range.

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