Very Short-Term Line Profile Variability in the Be Star π Aquarii

Details Very Short-Term Line Profile Variability in the Be Star π Aquarii Very Short-Term Line Profile Variability in the Be Star π Aquarii

Nov 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005aspc..337..294p&link_type=abstract

The Nature and Evolution of Disks Around Hot Stars, ASP Conference Series, Vol. 337, Proceedings of a meeting held 7-9 July 2004

Physics

2

Scientific paper

Short-term line profile variability observed in π Aqr during its recent non-emission phase has been analyzed using the technique of Gies & Kullavanijaya (1988). Data from three observing runs at the Kitt Peak National Observatory in 1999, 2000, and 2001 suggest that the star is pulsating in a nonradial ℓ=-m = 5 p mode with a period of ˜1.88 hr. The pulsations appear to be photospheric in origin, but significantly different than the half-day, low-order ℓ=-m = 2 g-mode activity observed in the Be star μ Cen during this star's non-emission episode in the 1980s and 1990s.

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