Open AccessExcitation and visibility of slow modes in rotating B‐type stars
Author(s) -
Dziembowski W. A.,
DaszyńskaDaszkiewicz J.,
Pamyatnykh A. A.
Publication year - 2007
Publication title -
monthly notices of the royal astronomical society
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 2.058
H-Index - 383
eISSN - 1365-2966
pISSN - 0035-8711
DOI - 10.1111/j.1365-2966.2006.11139.x
Subject(s) - physics , stars , visibility , excitation , instability , astrophysics , stability (learning theory) , space (punctuation) , rotation (mathematics) , mode (computer interface) , amplitude , optics , quantum mechanics , geometry , linguistics , philosophy , mathematics , machine learning , computer science , operating system
We use the traditional approximation to describe oscillations with frequencies comparable to the angular rotation rate. Validity of this approximation in application to main‐sequence B stars is discussed. Numerical results regarding mode stability and visibility are presented for a model of the Be star HD 163868. For this object, Walker et al. detected a record number of mode frequencies using data from the small space telescope MOST . Our interpretation of these data differs from that of Walker et al. In particular, we interpret peaks in the lowest frequency range as retrograde g modes. We find instability in a large number of modes that remain undetectable because of unfavourable aspect and/or effect of cancellation. There is no clear preference to excitation of prograde modes.