2016/02/10 by Th. Rivinius, R. H. D. Townsend, Rivinius, Th. +9
Physics and Astronomy · #FOS: Physical sciences #Solar and Stellar Astrophysics (astro-ph.SR) #astro-ph.SR
paper · pdf · doi:10.48550/arxiv.1602.03452
To appear in conference proceedings "Bright Emissaries: Be Stars as Messengers of Star-Disk Physics", eds. A. Sigut and C. Jones (11 Aug 2014 - 13 Aug 2014, London, Ontario, Canada)
arxiv created 2016/02/10 · arxiv updated 2016/02/11
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 π Aqr, are presented as well.