Variable rotational line broadening in the Be star Achernar

Aims. The main theoretical problem for the formation of a Keplerian disk around Be stars is how angular momentum is supplied\ud from the star to the disk, even more so since Be stars probably rotate somewhat subcritically. For instance, nonradial pulsation may\ud transport angular momentum to the stellar surface until (part of) this excess supports the disk-formation/replenishment. The nearby\ud Be star Achernar is presently building a new disk and o ers an excellent opportunity to observe this process from relatively close-up.\ud Methods. Spectra from various sources and epochs are scrutinized to identify the salient stellar parameters characterizing the disk life\ud cycle as defined by H emission. The variable strength of the non-radial pulsation is confirmed, but does not a ect the other results.\ud Results. For the first time it is demonstrated that the photospheric line width does vary in a Be star, by as much as v sin i . 35 km\ud However, unlike assumptions in which a photospheric spin-up accumulates during the diskless phase and then is released into the disk\ud as it is fed, the apparent photospheric spin-up is positively correlated with the appearance of H line emission. The photospheric\ud line widths and circumstellar emission increase together, and the apparent stellar rotation declines to the value at quiescence after the\ud H line emission becomes undetectableCNPq 307076/2012-1FAPESP 2010/19029-0NASA NNX12AC72