抄録
Using the Hα double peak emission lines of Pleione in the BeSS database from January 2009 to March 2023, the following points are discussed: 1) A comparison of the emission line profile variations observed at each periastron passage of the companion star reveals a striking similarity in the patterns of variation over the period 2015–2021. 2) As the periastron passage of the companion is repeated, the blue emission wing becomes stronger than the red emission wing towards the end of the Be-shell phase. 3) The mechanistic regularity whereby the red emission peak becomes earlier and stronger than the blue emission peak for a short time at each periastron passage of the companion star is interpreted qualitatively in terms of both the periastron position of the companion and the position of the disk in the celestial plane, as well as the tidal action of the companion star.
