# CONVECTION IN OBLATE SOLAR-TYPE STARS

@article{Wang2016CONVECTIONIO, title={CONVECTION IN OBLATE SOLAR-TYPE STARS}, author={Junfeng Wang and Mark S. Miesch and Chunlei Liang}, journal={The Astrophysical Journal}, year={2016}, volume={830} }

We present the first global 3D simulations of thermal convection in the oblate envelopes of rapidly rotating solar-type stars. This has been achieved by exploiting the capabilities of the new compressible high-order unstructured spectral difference (CHORUS) code. We consider rotation rates up to 85% of the critical (breakup) rotation rate, which yields an equatorial radius that is up to 17% larger than the polar radius. This substantial oblateness enhances the disparity between polar and…

## 5 Citations

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The star rotation will undoubtedly affect the star's characteristics described by the hydrostatic equilibrium equation. The centrifugal force distorts the star's shape and modifies its equilibrium…

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- PhysicsInternational Journal of Computational Fluid Dynamics
- 2021

When the high-order Spectral Difference (SD) method is used to discretize ideal magnetohydrodynamic (MHD) equations, it is challenging to satisfy the divergence-free constraint for the magnetic field…

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