Flux-Transport Dynamos with α-Effect from Global Instability of Tachocline Differential Rotation: A Solution for Magnetic Parity Selection in the Sun

By M. Dikpati, P. Gilman. 2001

224 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Molecular Biology

View Paper: https://www.semanticscholar.org/paper/f4784d8a20454e2fe909c30bd275a3e8f1920b49

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Citations in the corpus

Full-sphere simulations of a circulation-dominated solar dynamo: Exploring the parity issue (2004, methodology): “Some authors (Dikpati & Gilman 2001; Bonanno et al. 2002) obtained anti-solar quadrupolar modes in their calculations.”
Solar activity forecast with a dynamo model (2007, background): “If the diffusivity is low, then the dynamo solutions tend to be quadrupolar and one needs some additional ad hoc assumption like an extra α-effect at the bottom of the convection zone to make the solutions dipolar (Dikpati & Gilman 2001; Bonanno et al. 2002; Chatterjee et al. 2004).”
Dynamo processes and activity cycles of the active stars AB Doradus, LQ Hydrae and HR 1099 (2003, background): “…poloidal and toroidal fields vary in time with a phase shift roughly equal to 180◦ all over the surface, a very useful and challenging constraint for testing theoretical dynamo models (e.g. Rüdiger & Brandenburg 1995; Schlichenmaier & Stix 1995; Dikpati & Charbonneau 1999; Dikpati & Gilman 2001).”
Changes in Solar Dynamics from 1995 to 2002 (2002, background): “…dynamos suggest that the solar dynamo mechanism involves not only the above two processes but also an important third process, the advective transport of the magnetic flux by meridional circulation as in a conveyor belt (see Dikpati & Gilman 2001; Nandy & Choudhuri 2002 and references therein).”
Diagnostics of Polar Field Reversal in Solar Cycle 23 Using a Flux Transport Dynamo Model (2004, methodology): “The implications of such kinetic helicity in a dynamo model will be explored in a future paper, but in the present paper we stick to the profile used by Dikpati & Gilman (2001b).”
Evidence That a Deep Meridional Flow Sets the Sunspot Cycle Period (2003, background): “…convection (Parker 1955), decay of tilted bipolar sunspot pairs (Babcock 1961), buoyancy instability coupled with rotation (Brandenburg & Schmitt 1998), and hydrodynamic instability of the differential rotation (Dikpati & Gilman 2001), have been proposed to explain the origin of this -effect.”
Flux-Transport Dynamos with Lorentz Force Feedback on Differential Rotation and Meridional Flow: Saturation Mechanism and Torsional Oscillations (2006, methodology): “…dynamos have proven to be successful for modeling the evolution of the large scale solar magnetic field (Wang & Sheeley 1991; Durney 1995; Choudhuri et al. 1995; Dikpati & Charbonneau 1999; Küker et al. 2001; Dikpati & Gilman 2001; Dikpati et al. 2004; Dikpati 2005; Dikpati et al. 2006).”
Dynamo Models of the Solar Cycle (2005, methodology): “We now turn to a recently proposed class of dynamo models relying on the latitudinal shear instability of the angular velocity profiles in the upper radiative portion of the solar tachocline (Dikpati and Gilman, 2001).”
Magnetic Fields in the Solar Convection Zone (2004, background): “Fan (2009b) showed that the vortical motions in the two polarity flux concentrations twist up the inner emerged field lines, causing them to rotate in the atmosphere from an initial normal configuration (i.e. arching over the polarity inversion line from the positive to the negative polarity) into a”
Simulating and Predicting Solar Cycles Using a Flux-Transport Dynamo (2006, background): “Flux-transport-type solar dynamos (Wang & Sheeley 1991; Choudhuri et al. 1995; Durney 1995; Dikpati & Charbonneau 1999; Küker et al. 2001; Dikpati & Gilman 2001; Bonanno et al. 2002) have recently been successful in reproducing many solar cycle features, including the correct phase relationship…”
The solar magnetic field (2006, unknown): “Flux transport by meridional flow has also been considered in some models of overshoot-layer dynamos [184] and interface dynamos [185, 186].”
Astrophysical magnetic fields and nonlinear dynamo theory (2004, background): “Here the preferred modes have usually 11 quadrupolar symmetry about the equator rather than dipolar symmetry [355,356,428].”