Three-dimensional Spherical Simulations of Solar Convection. I. Differential Rotation and Pattern Evolution Achieved with Laminar and Turbulent States

By Mark S. Miesch, J. Elliott, J. Toomre, T. Clune, Gary A. Glatzmaier, P. Gilman. 2000

234 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Computational Mechanics, Molecular Biology

View Paper: https://www.semanticscholar.org/paper/8e2db37f62c6a6a15f3fb348997f7d33a2b98e91

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Citations in the corpus

Global-Scale Turbulent Convection and Magnetic Dynamo Action in the Solar Envelope (2004, methodology): “The Reynolds stresses are associated with correlations of the fluctuating velocity components which arise from organized tilts within the convective structures, especially in the downflow plumes (e.g. Brummell et al. 1998, Miesch et al. 2000).”
Turbulent Convection under the Influence of Rotation: Sustaining a Strong Differential Rotation (2002, methodology): “As discussed in detail in Miesch et al. (2000), these equations are fully nonlinear in velocity variables and linearized in thermodynamic variables with respect to a spherically symmetric mean state having a density ρ̄, pressure P̄ , temperature T̄ and specific entropy S̄ and perturbations about…”
Structure and Evolution of Giant Cells in Global Models of Solar Convection (2007, background): “Previous simulations which include convective penetration tend to exhibit equatorward meridional circulations throughout the lower convection zone and overshoot region (Miesch et al. 2000).”
Magnetic Field Generation in Fully Convective Rotating Spheres (2004, background): “Recent simulations still predict angular velocity to be roughly constant on cylinders, although some simulations show at least a tendency toward solar-like angular velocity contours (Miesch et al. 2000; Brun & Toomre 2002).”
MAGNETIC CYCLES IN GLOBAL LARGE-EDDY SIMULATIONS OF SOLAR CONVECTION (2010, methodology): “Following the advent of high-performance computing, parallelized versions of the Glatzmaier simulation model (Clune et al. 1999) made possible much higher resolution runs attaining a strongly turbulent regime (Miesch et al. 2000).”
Ephemeral Regions on a Sequence of Full-Disk Michelson Doppler Imager Magnetograms (2001, background): “The locations where Ñux emerges may form a pattern with a larger scale, as suggested by Beck, Duvall, & Scherrer (1998), and simulated by Miesch et al. (2000).”
Flux-Transport Dynamos with Lorentz Force Feedback on Differential Rotation and Meridional Flow: Saturation Mechanism and Torsional Oscillations (2006, unknown): “…have been addressed in the past mainly through two approaches: 3D full spherical shell simulations (Glatzmaier & Gilman 1982; Gilman & Miller 1986; Miesch et al. 2000; Brun & Toomre 2002) and axisymmetric meanfield models (Kitchatinov & Rüdiger 1993, 1995; Rüdiger et al. 1998; Küker & Stix…”
Full-sphere simulations of a circulation-dominated solar dynamo: Exploring the parity issue (2004, methodology): “This view is supported by recent simulations of solar convection (Miesch et al. 2000).”
Dynamo Action in the Solar Convection Zone and Tachocline: Pumping and Organization of Toroidal Fields (2006, methodology): “We adopt a softer subadiabatic stratification in the lower stable zone to ease our numerical resolution of internal gravity waves produced by the overshooting motions (see Miesch et al. 2000).”
Simulations of Dynamo Action in Fully Convective Stars (2007, methodology): “…gradient in equation (4) is most justifiable in convection zones, where the stratification will tend toward adiabaticity; in stable zones, this term should be modified in order to avoid spuriously large SGS heat fluxes directed radially inwards (as discussed in Miesch 1998; Miesch et al. 2000).”
Solar Differential Rotation Influenced by Latitudinal Entropy Variations in the Tachocline (2006, background): “…to be more cylindrical (angular velocity contours parallel to the rotation axis) than conical (radial angular velocity contours) (e.g., Gilman 1977, 1978; Glatzmaier 1984; Gilman & Miller 1986; Miesch et al. 2000; Elliott et al. 2000; Robinson & Chan 2001; Brun & Toomre 2002; Brun et al. 2004).”
Anelastic convection-driven dynamo benchmarks (2011, background): “…and so allows a much larger timestep, is therefore a popular choice for studies of solar and stellar convection zones and the interior dynamics of giant planets (e.g. Glatzmaier, 1984, 1985; Brun et al., 2004; Jones et al., 2009; Jones and Kuzanyan, 2009; Miesch et al., 2000; Kaspi et al., 2009).”
Evolving Submerged Meridional Circulation Cells within the Upper Convection Zone Revealed by Ring-Diagram Analysis (2002, background): “The transitory nature of this undulatory pattern is typical of the convective structures that are seen in numerical simulations of turbulent solar convection (e.g., Miesch et al. 2000; Brun & Toomre 2001).”
Simulations of Core Convection in Rotating A-Type Stars: Differential Rotation and Overshooting (2003, methodology): “We are encouraged, however, by the success that similar simulations (e.g., Miesch et al. 2000; Elliott et al. 2000; Brun & Toomre 2002) have enjoyed in matching the detailed observational constraints for the differential rotation within the solar convection zone provided by helioseismology.”
Stochastic Fluctuations in a Babcock-Leighton Model of the Solar Cycle (2000, methodology): “This expectation is certainly borne out by observations of the solar surface meridional Ñow as well as numerical simulations, with both suggesting rms Ñuctuations comparable to, or even exceeding, the mean meridional Ñow speed (Hathaway 1996 ; Miesch et al. 2000).”
Penetration and Overshooting in Turbulent Compressible Convection (2002, background): “…to reproduce in self-consistent models (Gilman 1975, 1977; Glatzmaier & Gilman 1981a, 1981b; Glatzmaier 1984, 1985a, 1985b; Gilman & Miller 1986; Miesch et al. 2000; Elliott, Miesch, & Toomre 2000), and the cause of the solid-body rotation of the radiative core has prompted much diverse…”