Spectrophotometry of OH 26.5+0.6 from 2 to 40 microns. (original) (raw)

NASA/ADS

;

• Gillett, F. C. ;
• Houck, J. R. ;
• McCarthy, J. F. ;
• Merrill, K. M. ;
• Pipher, J. L. ;
• Puetter, R. C. ;
• Russell, R. W. ;
• Soifer, B. T. ;
• Willner, S. P.

Abstract

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.

Publication:

The Astrophysical Journal

Pub Date:

January 1978

DOI:

10.1086/155760

Bibcode:

1978ApJ...219..114F

Keywords:

• 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;
• Astronomy;
• Absorption Lines:OH Sources;
• Circumstellar Envelopes:OH Sources;
• Infrared Radiation:OH Sources;
• OH Sources:Models;
• OH Sources:Spectrophotometry