Spectroscopic and photometric observations of the IRAS source 20056+1834 are discussed. The optical counterpart has a visual magnitude of 12.5 and its spectrum appears to be that of a G0 supergiant on which are superimposed very strong, broad (140 km s−1 FWHM) Na D emission lines. Photometrically the object varies with a low amplitude and a characteristic time-scale of 50 days. A model is proposed in which a mass-losing star is obscured from direct view by a thick dust cloud so that its photosphere is seen only in reflection. The Na D emission is produced by resonantly scattered starlight in the expanding, unobscured stellar envelope.
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Menzies et al. (1988) studied this question.