Deep photospheric flows in tau Scorpii

From analysis of weak, unblended, ultraviolet lines observed in tau Scorpii by Copernicus, we find the same line widths and the same slightly blue-depressed wings as found in the upper photospheric lines of the visual region. In addition, we find a radial velocity discrepancy of about 6 km s-1 between weak and strong lines in the l000 A--1300 A region. These results are in quantitative agreement with one another and with the results of the visual region. They imply that a flow of material is present even in the deep photosphere of this star. However, one cannot yet specify the geometry of the flow (outward-radial versus temperature-weighted convection columns).At the least, this flow alters the expected radiation-driven flow solution close to the photosphere. At most, it could provide the heating of a chromosphere or a corona just outside the photosphere, as required by the imperfect flow model