Rapidly Rotating Suns and Active Nests of Convection

@article{Brown2008RapidlyRS,
  title={Rapidly Rotating Suns and Active Nests of Convection},
  author={Benjamin P. Brown and Matthew Keith Morris Browning and Allan Sacha Brun and Mark S. Miesch and Juri Toomre Jila and Dept. AstrophysicalPlanetary Sciences and University of Colorado and Boulder and CO Dept. of Astronomy and University of Southern California and Berkeley and CA DSMIRFUSAp and CEA-SaclayUMR Aim and 7 CEA-CNRS-UniversiteParis and Gif-sur-Yvette. and France High Altitude Observatory and Ncar and Co},
  journal={The Astrophysical Journal},
  year={2008},
  volume={689},
  pages={1354-1372}
}
  • B. Brown, M. Browning, Co
  • Published 12 August 2008
  • Physics, Environmental Science
  • The Astrophysical Journal
In the solar convection zone, rotation couples with intensely turbulent convection to drive a strong differential rotation and achieve complex magnetic dynamo action. Our Sun must have rotated more rapidly in its past, as is suggested by observations of many rapidly rotating young solar-type stars. Here we explore the effects of more rapid rotation on the global-scale patterns of convection in such stars and the flows of differential rotation and meridional circulation, which are self… 
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TLDR
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Theory of differential rotation and meridional circulation
  • L. Kitchatinov
  • Physics, Environmental Science
    Proceedings of the International Astronomical Union
  • 2012
Abstract Meridional flow results from slight deviations from the thermal wind balance. The deviations are relatively large in the boundary layers near the top and bottom of the convection zone.
Solar differential rotation reproduced with high-resolution simulation
The Sun rotates differentially with a fast equator and slow pole[1]. Convection in the solar interior is thought to maintain the differential rotation. However, although many numerical simulations
Stellar Midlife Crises: Challenges and Advances in Simulating Convection and Differential Rotation in Sun-like Stars
Abstract Low mass, main sequence stars like our Sun exhibit a wide variety of rotational and magnetic states. Observational and theoretical advances have led to a renewed emphasis on understanding
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