Full-sphere simulations of a circulation-dominated solar dynamo: Exploring the parity issue

By Piyali Chatterjee, Dibyendu Nandy, A. Choudhuri. 2004

195 citations recorded by the source corpus.

We explore a two-dimensional kinematic solar dynamo model in a full sphere, based on the helioseismically determined solar rotation profile and with an α effect concentrated near the solar surface, which captures the Babcock-Leighton idea that the poloidal field is created from the decay of tilted bipolar active regions. The meridional circulation, assumed to penetrate slightly below the tachocline, plays an important role. Some doubts have recently been raised regarding the ability of such a model to reproduce olar-like dipolar parity. We specifically address the parity issue and show that the dipolar mode is preferred when certain reasonable conditions are satisfied, the most important condition being the requirement that the poloidal field should diffuse efficiently to get coupled across the equator. Our model is shown to reproduce various aspects of observational data, including the phase relation between sunspots and the weak, diffuse field.

Subfields: Astronomy and Astrophysics, Computational Mechanics, Statistical and Nonlinear Physics

View Paper: https://www.semanticscholar.org/paper/e2a3370a394fa007b84fd0666898fb460ce55918

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Citations in the corpus

Dynamo Models of the Solar Cycle (2005, background): “…over a full meridional plane (see, e.g., Dikpati and Gilman, 2001), but it is not clear how serious a problem this is, as relatively minor changes to the model input ingredients may flip the dominant parity (see, e.g., Chatterjee et al., 2004, for a specific, if physically curious, example).”
Astrophysical magnetic fields and nonlinear dynamo theory (2004, background): “The resulting butterfly diagram is quite realistic [426], although the parity issue remains 17 to be clarified [356,429].”
Solar activity forecast with a dynamo model (2007, methodology): “Most of our calculations are based on the dynamo model presented by Nandy & Choudhuri (2002) and Chatterjee et al. (2004).”
Magnetic Flux Transport at the Solar Surface (2014, methodology): “In some Babcock-Leighton type dynamo models (e.g., Chatterjee et al. 2004; Jiang et al. 2013b), this correlation exists because the poloidal field generated by the surface flux transport can be quickly transported to the tachocline where it gets wound up by the differential rotation to produce the…”
The Case for a Distributed Solar Dynamo Shaped by Near-Surface Shear (2005, methodology): “A different class of models are the Babcock-Leighton type flux transport dynamos, as recently studied by Dikpati & Charbonneau (1999), Nandy & Choudhuri (2002), and Chatterjee et al. (2004).”
Solar Dynamo Theory (2014, methodology): “…Babcock-Leighton mechanism, required here because a fundamentally nonaxisymmetric process must be “forced” into a global axisymmetric model (see, e.g., Durney 1995, Dikpati & Charbonneau 1999, Nandy & Choudhuri 2001, Chatterjee et al. 2004, Charbonneau et al. 2005, Muñoz-Jaramillo et al. 2010).”
Exploring the Physical Basis of Solar Cycle Predictions: Flux Transport Dynamics and Persistence of Memory in Advection- versus Diffusion-dominated Solar Convection Zones (2007, methodology): “We use the solar dynamo code Surya, which has been studied extensively in different contexts (e.g. Nandy & Choudhuri 2002, Chatterjee et al. 2004, Chatterjee & Choudhuri 2006), and is made available to the public on request.”