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arXiv · 1309.7286

Variable rotational line broadening in the Be star Achernar

Th. Rivinius·D. Baade·R. H. D. Townsend·A. C. Carciofi·S. Štefl
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Abstract

The main theoretical problem for the formation of a Keplerian disk around Be stars is how to supply angular momentum from the star to the disk, even more so since Be stars probably rotate somewhat sub-critically. For instance, nonradial pulsation may transport angular momentum to the stellar surface until (part of) this excess supports the disk formation/replenishment. The nearby Be star Achernar is presently building a new disk and offers an excellent opportunity to observe this process from relatively close-up. Spectra from various sources and epochs are scrutinized to identify the salient stellar parameters characterizing the disk life cycle as defined by H\alpha emission. Variable strength of the non-radial pulsation is confirmed, but does not affect the further results. For the first time it is demonstrated that the photospheric line width does vary in a Be star, by as much as \Delta v sin i \lesssim 35kms^{-1}. However, contrary to assumptions in which a photospheric spin-up accumulates during the diskless phase and then is released into the disk as it is fed, the apparent photospheric spin-up is positively correlated with the appearance of H\alpha line emission: The photospheric line widths and circumstellar emission increase together, and the apparent stellar rotation declines to the value at quiescence after the H\alpha line emission becomes undetectable.

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Th. Rivinius, D. Baade, R. H. D. Townsend, A. C. Carciofi, S. Štefl. 2013-09-27. Variable rotational line broadening in the Be star Achernar. https://doi.org/10.1051/0004-6361/201322515

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