[en] The strength of this weak absorption feature appears to depend upon the strength of the primary line but not on the excitation potential or ion stage. The feature appears to be due neither to an instrumental artifact nor to the presence of a secondary star. It is concluded that in both stars there is a flow moving upward at 8.6 +- 1.4 km s^-1 (about the sonic velocity) in the atmosphere. This finding has wide ramifications for any assumption involving hydrostatic equilibium or stability in the atmospheres of such stars