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Two-dimensional simulations of internal gravity waves in the radiation zones of intermediate-mass stars

Lookup NU author(s): Rathish Ratnasingam, Dr Philipp Edelmann, Professor Tamara Rogers


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© 2020 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society. Intermediate-mass main-sequence stars have large radiative envelopes overlying convective cores. This configuration allows internal gravity waves (IGWs) generated at the convective-radiative interface to propagate towards the stellar surface. The signatures of these waves can be observed in the photometric and spectroscopic data from stars. We have studied the propagation of these IGWs using two-dimensional (2D) fully non-linear hydrodynamical simulations with realistic stellar reference states from the 1D stellar evolution code, Modules for Stellar Astrophysics (mesa). When a single wave is forced, we observe wave self-interaction. When two waves are forced, we observe non-linear interaction (i.e. triadic interaction) between these waves forming waves at different wavelengths and frequencies. When a spectrum of waves similar to that found in numerical simulations is forced, we find that the surface IGW frequency slope is consistent with recent observations. This power law is similar to that predicted by linear theory for the wave propagation, with small deviations that can be an effect of non-linearities. When the same generation spectrum is applied to 3 M⊙ models at different stellar rotation and ages, the surface IGW spectrum slope is very similar to the generation spectrum slope.

Publication metadata

Author(s): Ratnasingam RP, Edelmann PVF, Rogers TM

Publication type: Article

Publication status: Published

Journal: Monthly Notices of the Royal Astronomical Society

Year: 2020

Volume: 497

Issue: 4

Pages: 4231-4245

Print publication date: 01/10/2020

Online publication date: 07/08/2020

Acceptance date: 29/07/2020

ISSN (print): 0035-8711

ISSN (electronic): 1365-2966

Publisher: Oxford University Press


DOI: 10.1093/mnras/staa2296


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