Non-radial pulsations in the O stars XI Persei and lambda Cephei

Details Non-radial pulsations in the O stars XI Persei and lambda Cephei Non-radial pulsations in the O stars XI Persei and lambda Cephei

May 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999a%26a...345..172d&link_type=abstract

Astronomy and Astrophysics, v.345, p.172-180 (1999)

Astronomy and Astrophysics

Astrophysics

33

Stars: Early-Type, Stars: Individual: Xi Per, Stars: Individual: Lambda Cep, Stars: Mass-Loss, Stars: Winds, Outflows

Scientific paper

A new time-series analysis of profile changes in the photospheric He I lambda 4713 spectral line from data taken during 5 days in 1989 at the Calar Alto and Kitt Peak observatories has provided evidence for the presence of a non-radial prograde p-mode in the O 7.5 giant xi Per (l = 3, P = 3.5) and probably two such modes in the O6 supergiant lambda Cep (l = 3, P = 12.3 h and l = 5, P = 6.6 h). The corotating pulsation periods are in both cases much shorter than the estimated stellar rotation period. Modeling the observed amplitude of the line-profile changes (assuming |m|=l) yields a velocity amplitude of approximately 5 km s(-1) of the pulsation in xi Per and 6 km s(-1) in lambda Cep. Any such a pulsation by itself is unlikely to be the cause of the well-known cyclical wind variability in these stars because the pulsation period is too short, but the cumulative action of multiple modes could cause such an effect. Weak magnetic fields anchored at the surface remain the strongest candidate for the origin of wind variability.

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