On the Interaction between Convection and Magnetic Fields

By F. Cattaneo, Thierry Emonet, N. Weiss. 2003

240 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Molecular Biology, Physiology

View Paper: https://www.semanticscholar.org/paper/e882bdffecbb89c3e0bb3d29528a2111d89658f1

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Solar Dynamo Theory (2014, background): “A turbulent flow can generate strong magnetic fields on its own small spatial scale provided Rm is large enough (see, e.g., Cattaneo 1999, Cattaneo et al. 2003, Stein & Nordlund 2006, Vögler & Schüssler 2007).”
A solar surface dynamo (2007, background): “The principle of such a non-helical surface dynamo has been demonstrated in incompressible closed-box MHD simulations of thermal convection at high Rayleigh number (Cattaneo, 1999; Cattaneo et al., 2003).”
Magnetic Fields in the Solar Convection Zone (2004, background): “The twist may be due to the current helicity in the dynamo generated toroidal magnetic field, from which buoyant flux tubes form at the base of the convection zone (Gilman and Charbonneau, 1999), or it may be acquired during the rise of the flux tubes through the solar convection zone (Longcope et a”
HEATING OF THE SOLAR CHROMOSPHERE AND CORONA BY ALFVÉN WAVE TURBULENCE (2011, background): “This is plausible because the flux tubes are sur- rounded by convective downflows that are highly turbulent (Cattaneo et al. 2003; Vögler et al. 2005; Stein & Nordlund 2006; Bushby et al. 2008).”
Dynamo Models of the Solar Cycle (2005, background): “The culprit is most likely the generation of small-scale magnetic fields by these turbulent fluid motions (see, e.g., Cattaneo, 1999; Cattaneo et al., 2003, and references therein).”
The Sun’s Supergranulation (2010, background): “Only in the presence of a strong mean vertical field is the peak horizontal scale of these turbulent convective motions strongly constrained and reduced bymagnetic tension (Tao et al. 1998; Cattaneo et al. 2003).”
Fluctuation dynamo and turbulent induction at low magnetic Prandtl numbers (2007, methodology): “…et al. 2003, Socas-Navarro & Lites 2004, Trujillo Bueno et al. 2004, Solanki et al. 2006), the numerical evidence used to argue that the turbulent fluctuation dynamo is responsible has thus far been based on numerical simulations with Pm ≥ 1 (Cattaneo 1999, Cattaneo et al. 2003, Bushby 2007).”
Simulations of magneto-convection in the solar photosphere Equations, methods, and results of the MURaM code (2005, methodology): “Following the lines of more idealized models, Cattaneo (1999), Emonet & Cattaneo (2001) and Cattaneo et al. (2003) have carried out simulations of thermal magneto-convection in the Boussinesq approximation which highlighted the possibility that a substantial fraction of the magnetic field in the…”
Oscillations and Waves in Sunspots (2015, background): “…sunspot’s umbrae and penumbrae, magnetoconvection models indicate that these environments can be convective (Savage, 1969; Moore, 1973; Lee, 1993; Weiss et al., 1990; Cattaneo et al., 2003; Schüssler and Vögler, 2006; Spruit and Scharmer, 2006), see the review by Rempel and Schlichenmaier (2011).”
Numerical Modeling of Magnetohydrodynamic Wave Propagation and Refraction in Sunspots (2006, background): “On the one hand, these sources can be due to the presence of a weak convection that can generate waves directly inside the umbral atmosphere (see, e.g., Weiss et al. 1990; Cattaneo et al. 2003).”
Heat transfer and large scale dynamics in turbulent Rayleigh-Bénard convection (2008, background): “In the geophysical and astrophysical context, we mention convection in Earth’s mantle (see e.g. McKenzie et al. (1974)), in Earth’s outer core (see e.g. Cardin and Olson (1994)), and in stars including our sun (see e.g. Cattaneo et al. (2003)).”