Journal
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
Volume 469, Issue 1, Pages 13-46Publisher
OXFORD UNIV PRESS
DOI: 10.1093/mnras/stx738
Keywords
stars: early-type -stars: oscillations; stars: rotation
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Funding
- Polish National Science Centre [2015/17/B/ST9/02082]
- Wroclaw Centre for Networking and Supercomputing [265]
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We determine instability domains on the Hertzsprung-Russell diagram for rotating main sequence stars with masses of 2-20 M-circle dot. The effects of the Coriolis force are treated wihin the traditional approximation. High-order g modes with harmonic degrees l up to 4 and mixed gravity-Rossby modes with vertical bar m vertical bar up to 4 are considered. We include the effects of rotation in wider instability strips for a given l compared to the non-rotating case and in an extension of the pulsational instability to hotter and more massive models. We present results for a fixed value of the initial rotation velocity as well as for a fixed ratio of the angular rotation frequency to its critical value. Moreover, we check how the initial hydrogen abundance, metallicity, overshooting from the convective core and opacity affect the pulsational instability domains. The effect of rotation on the period spacing is also discussed.
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