Document Type
Peer-Reviewed Article
Publication Date
7-2020
Abstract
This paper presents the results of a set of radiative hydrodynamic (RHD) simulations of convection in the near-surface regions of a rapidly rotating star. The simulations use microphysics consistent with stellar models, and include the effects of realistic convection and radiative transfer. We find that the overall effect of rotation is to reduce the strength of turbulence. The combination of rotation and radiative cooling creates a zonal velocity profile in which the motion of fluid parcels near the surface is independent of rotation. Their motion is controlled by the strong up and down flows generated by radiative cooling. The fluid parcels in the deeper layers, on the other hand, are controlled by rotation.
DOI
10.1093/mnras/staa1507
Recommended Citation
Robinson, F. J., Tanner, J., & Basu, S. (2020). Simulating the outer layers of rapidly rotating stars. Monthly Notices of the Royal Astronomical Society, 495(4), 5052-5059. Doi: 10.1093/mnras/staa1507
Creative Commons License
This work is licensed under a Creative Commons Attribution-NonCommercial-No Derivative Works 4.0 International License.
Comments
© 2020 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society.
Version posted is the authors' Preprint 27 May 2020.