  Spectroscopic observations of Achernar over the past decades, have shown the
photospheric line width, as measured by the rotational parameter $v \sin i$, to
vary in correlation with the emission activity. Here we present new
observations, covering the most recent activity phase, and further archival
data collected from the archives. The $v \sin i$ variation is confirmed. On the
basis of the available data it cannot be decided with certainty whether the
increased line width precedes the emission activity, i.e. is a signature of the
ejection mechanism, or postdates is, which would make it a signature of
re-accretion of some of the disk-material. However, the observed evidence leans
towards the re-accretion hypothesis. Two further stars showing the effect of
variable line width in correlation with emission activity, namely 66 Oph and
$\pi$ Aqr, are presented as well.
