Solar Differential Rotation Influenced by Latitudinal Entropy Variations in the Tachocline

By Mark S. Miesch, A. Brun, J. Toomre. 2006

229 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Atmospheric Science, Global and Planetary Change

View Paper: https://www.semanticscholar.org/paper/781c83387d3e5b80fbae6768e173e80c1e76c792

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

1. Paul Charbonneau
2. Mark S. Miesch
3. J. Toomre
4. A. Brun
5. M. Browning
6. Matthias Rempel
7. Benjamin P. Brown
8. D. Hathaway

In Atmospheric Science

1. M. Browning
2. Mark S. Miesch
3. A. Brun
4. J. Toomre
5. Paul Charbonneau

In Global and Planetary Change

1. M. Browning
2. J. Toomre
3. Mark S. Miesch
4. A. Brun
5. Paul Charbonneau

Citations in the corpus

• DETECTION OF EQUATORWARD MERIDIONAL FLOW AND EVIDENCE OF DOUBLE-CELL MERIDIONAL CIRCULATION INSIDE THE SUN (2013, background): “However, on the other hand, solar convection simulations have shown the possibility of multi-cell circulation with a shallow equatorward flow (e.g., Miesch et al. 2006; Käpylä et al. 2012; Guerrero et al. 2013), demonstrating that our analysis results are reasonable.”
• Structure and Evolution of Giant Cells in Global Models of Solar Convection (2007, methodology): “This difference may arise from viscous diffusion which, although lower than in previous models is still higher than in the Sun, or from thermal and mechanical coupling to the tachocline which is only crudely incorporated into this model through our lower boundary conditions (Miesch et al. 2006).”
• PERSISTENT MAGNETIC WREATHS IN A RAPIDLY ROTATING SUN (2010, background): “The tilt ofΩ contours in the Sun may be due in part to the thermal structure of the solar tachocline, as first found in the mean-field models of Rempel (2005) and then in 3D simulations of global-scale convection by Miesch et al. (2006).”
• MAGNETIC CYCLES IN A CONVECTIVE DYNAMO SIMULATION OF A YOUNG SOLAR-TYPE STAR (2011, background): “The main effect is to tilt theΩ contours toward a more radial alignment (Rempel 2005; Miesch et al. 2006).”
• Solar Dynamo Theory (2014, background): “…this deviation from cylindrical isocontours is now understood to be caused by a latitudinal entropy gradient present throughout the convection zone, which results in a thermal wind balance that breaks the Taylor-Proudman theorem (Kitchatinov & Rudiger 1995, Miesch et al. 2006, Balbus et al. 2009).”
• Simulations of Dynamo Action in Fully Convective Stars (2007, background): “It is difficult to estimate the impacts each of these may have, but we are encouraged by the reasonable success that similar simulations of the solar interior have enjoyed in matching the detailed observational constraints provided by helioseismology (Miesch et al. 2006; Browning et al. 2006).”
• Simulating and Predicting Solar Cycles Using a Flux-Transport Dynamo (2006, background): “Recently, Miesch et al. (2006) took guidance from the mean field model results of Rempel et al. (2005) to significantly improve their three-dimensional HD numerical simulations of the differential rotation of the Sun.”
• Dynamo Action in the Solar Convection Zone and Tachocline: Pumping and Organization of Toroidal Fields (2006, result): “Recent studies of the interaction of turbulent convection with rotation (e.g., Miesch et al. 2000, 2006; Brun & Toomre 2002) now yield global differential rotation profiles in close accord with helioseismic deductions (e.g., Thompson et al. 2003) in the bulk of the convection zone.”
• MAGNETIC WREATHS AND CYCLES IN CONVECTIVE DYNAMOS (2012, background): “Miesch et al. (2006, 2008) have explored the interplay of rotation, stratification, and moderately turbulent convection to produce strong differential rotation in a hydrodynamic setting.”