The Dwarf Binary HD 16157 : An Interim Report

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Abstract
Spectroscopic observations of this remarkable star have been carried on since 1951 using the equipment of the Radcliffe Observatory, Pretoria. It now seems tolerably certain that it is a spectroscopic binary, of which the primary component is a late K-type dwarf, having an orbital period of 1.56145 days, and a mass function with the very low value of 0.00871 solar masses. On a few plates evidence of the spectrum of the secondary component is thought to have been found. The parallax has been measured as 0″.083. The spectra resemble those of YY Geminorum in showing Balmer lines and Calcium lines in emission. The star also resembles YY Geminorum in the fact that it is also a light variable showing changes in the light curve from season to season which are even more pronounced than those shown by the latter. It seems difficult to account for these in terms of the ordinary eclipsing binary model, and the data which have been obtained so far are presented with the object of encouraging independent observations elsewhere.

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