Transport and Storage of Magnetic Field by Overshooting Turbulent Compressible Convection

By S. Tobias, N. Brummell, T. Clune, J. Toomre. 2001

207 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Molecular Biology

View Paper: https://www.semanticscholar.org/paper/5a4930aedebbf1981a19413159203a6ba28fafd4

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Citations in the corpus

Dynamo Models of the Solar Cycle (2005, background): “A number of attempts have also been made to reproduce some salient features of the solar cycle by carrying out high-resolution, local simulations in parameters regimes closer to solar-like (see, e.g., Nordlund et al., 1992; Tobias et al., 2001; Ossendrijver et al., 2002).”
Global-Scale Turbulent Convection and Magnetic Dynamo Action in the Solar Envelope (2004, background): “Many of the main features are qualitatively similar to simulations of turbulent, compressible magnetoconvection in Cartesian geometries (Cattaneo 1999; Stein & Nordlund 2000; Tobias et al. 2001).”
The Case for a Distributed Solar Dynamo Shaped by Near-Surface Shear (2005, background): “…is strongly offset by the action of turbulent pumping, which leads to a net accumulation of magnetic energy at the bottom of the convection zone (Nordlund et al. 1992, Brandenburg et al. 1996, Tobias et al. 1998, 2001, Dorch & Nordlund 2001, Ossendrijver et al. 2002, Ziegler & Rüdiger 2003).”
Magnetic flux emergence in granular convection: radiative MHD simulations and observational signatures (2007, background): “The behaviour of the flux tube in the presence of asymmetrical up- and down-flows in compressible convection is reminiscent of the turbulent pumping mechanism studied by Tobias et al. (2001).”
Solar Dynamo Theory (2014, background): “All three simulations show significant accumulation of magnetic field at the base of the convecting layers, as expected of turbulent convection in a stratified environment (e.g., Tobias et al. 2001).”
Exploring the Physical Basis of Solar Cycle Predictions: Flux Transport Dynamics and Persistence of Memory in Advection- versus Diffusion-dominated Solar Convection Zones (2007, background): “We may also point out that in the context of cycle-tocycle correlations, downward flux pumping (Tobias et al. 2001) would have the same effect as diffusion in that it also acts to short-circuit the meridional circulation conveyor belt.”
Penetration and Overshooting in Turbulent Compressible Convection (2002, background): “This significant change is of interest, since the mixing of passive fields, such as chemical abundances or even active ingredients, such as magnetic fields (Tobias et al. 1998, 2001), may be influenced by these dramatic events.”
Astrophysical magnetic fields and nonlinear dynamo theory (2004, background): “have allowed a more quantitative description of the pumping effect and the associated pump velocity 1 [332,333].”
Turbulent Convection under the Influence of Rotation: Sustaining a Strong Differential Rotation (2002, background): “…into stable domains below (Brummell et al. 2001, Porter & Woodward 2001), of effects of realistic near-surface physics on granulation and supergranulation (e.g. Stein & Nordlund 1998), and of dynamo processes and magnetic transport by the convection (e.g. Cattaneo 1999, Tobias et al. 2001).”
The Internal Rotation of the Sun (2003, background): “…and storing magnetic flux, so magnetism likely plays a more substantial 1 Aug 2003 14:6 AR AR194-AA41-15.tex AR194-AA41-15.sgm LaTeX2e(2002/01/18)P1: GCE 634 THOMPSON ET AL. dynamical role here than in the overlying envelope (e.g., Ferriz-Mas 1996, Gilman 2000a, Stix 1991, Tobias et al. 2001).”
On the Interaction between Convection and Magnetic Fields (2003, background): “…(Meneguzzi & Pouquet 1989; Cattaneo 1999; Thelen & Cattaneo 2000; Cattaneo, Lenz, & Weiss 2001; Emonet & Cattaneo 2001), magnetoconvection (see, e.g., Tao et al. 1998; Rucklidge et al. 2000; Weiss et al. 2002), or flux pumping (Tobias et al. 1998, 2001; Dorch & Nordlund 2001), regarded separately.”
Magnetic Fields in the Solar Convection Zone (2004, methodology): “𝐵eq out of the convection zone into the stable overshoot region demonstrated by the high resolution 3D MHD simulations has profound implications for the working of the interface mean field dynamo models (Parker, 1993; Charbonneau and MacGregor, 1997) as discussed by Tobias et al. (2001).”