The solar dynamo

Miesch, Mark S.

doi:10.1098/rsta.2011.0507

Cited by 46 publications

(21 citation statements)

References 84 publications

(147 reference statements)

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“…The view is from above the north pole, with the tube located near the equator (latitude approximately 15 • ). Colors along the tube indicate density, from low (red/orange) to high (blue) while background colors indicate convective downflows (blue) and upflows (red) dynamical quenching associated with the small-scale accumulation of magnetic helicity, boundary conditions, and the nature of the artificial dissipation, be it an explicit subgridscale model or an implicit numerical diffusion (see reviews by Brandenburg and Subramanian 2005;Miesch 2012;Tobias et al 2013;Charbonneau 2013). Furthermore, though extracting mean-field coefficients from convective dynamo models is an auspicious endeavor for the future, there are times when simple mean-field prescriptions may not provide a reliable depiction of the convective field generation and transport processes (e.g.…”

Section: Convective Transport and Dynamo Actionmentioning

confidence: 99%

Flux Transport Dynamos: From Kinematics to Dynamics

et al. 2014

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Over the past several decades, Flux-Transport Dynamo (FTD) models have emerged as a popular paradigm for explaining the cyclic nature of solar magnetic activity. Their defining characteristic is the key role played by the mean meridional circulation in transporting magnetic flux and thereby regulating the cycle period. Most FTD models also incorporate the so-called Babcock-Leighton (BL) mechanism in which the mean poloidal field is produced by the emergence and subsequent dispersal of bipolar active regions. This feature is well grounded in solar observations and provides a means for assimilating observed surface flows and fields into the models in order to forecast future solar activity, to identify model biases, and to clarify the underlying physical processes. Furthermore, interpreting historical sunspot records within the context of FTD models can potentially provide insight into why cycle features such as amplitude and duration vary and what causes extreme events such as Grand Minima. Though they are generally robust in a modeling sense and make good contact with observed cycle features, FTD models rely on input physics that B.B. Karak et al. is only partially constrained by observation and that neglects the subtleties of convective transport, convective field generation, and nonlinear feedbacks. Here we review the formulation and application of FTD models and assess our current understanding of the input physics based largely on complementary 3D MHD simulations of solar convection, dynamo action, and flux emergence.

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Section: Convective Transport and Dynamo Actionmentioning

confidence: 99%

Flux Transport Dynamos: From Kinematics to Dynamics

et al. 2014

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“…Global dynamos have been simulated by Miesch [34], Brun et al [82], Dobler et al [83], Browning et al [84] and Brown et al [85,86]. See also the review by Miesch [44]. Note that the fact that both the rate of magnetic flux emergence and the probability distribution of magnetic flux magnitudes are featureless power laws from 10 16 to 10 23 Mx suggests that the solar dynamo has no preferred scale, and that it acts throughout the convection zone with each scale of convective motions generating new flux on that scale [45,87].…”

Section: (C) Dynamo Actionmentioning

confidence: 99%

“…The third starts from a tiny seed field in the initial convective state and is used to study dynamo action, sometimes in a small localized setting, sometimes on the global scale of the entire Sun. The solar dynamo is discussed by Miesch [44] and sunspots by Rempel [53] in this series. Here, we review flux emergence and quiet Sun magneto-convection simulations.…”

Section: Simulationsmentioning

confidence: 99%

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Magneto-convection

Stein

2012

Phil. Trans. R. Soc. A.

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Convection is the transport of energy by bulk mass motions. Magnetic fields alter convection via the Lorentz force, while convection moves the fields via the curl(v × B) term in the induction equation. Recent ground-based and satellite telescopes have increased our knowledge of the solar magnetic fields on a wide range of spatial and temporal scales. Magneto-convection modelling has also greatly improved recently as computers become more powerful. Three-dimensional simulations with radiative transfer and non-ideal equations of state are being performed. Flux emergence from the convection zone through the visible surface (and into the chromosphere and corona) has been modelled. Local, convectively driven dynamo action has been studied. The alteration in the appearance of granules and the formation of pores and sunspots has been investigated. Magneto-convection calculations have improved our ability to interpret solar observations, especially the inversion of Stokes spectra to obtain the magnetic field and the use of helioseismology to determine the subsurface structure of the Sun.

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“…Instead, turbulent convection operates in a highly complex system where rotational shear, global circulation and boundary conditions on local and global scales are all important. Miesch [3], describes the complexities behind the generation mechanisms of the Sun's magnetic field and explains the circulatory patterns within the solar interior.…”

Section: Dynamos and Magneto-convectionmentioning

confidence: 99%

Astrophysical processes on the Sun

Parnell

2012

Phil. Trans. R. Soc. A.

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Over the past two decades, there have been a series of major solar space missions, namely Yohkoh, SOHO, TRACE, and in the past 5 years, STEREO, Hinode and SDO, studying various aspects of the Sun and providing images and spectroscopic data with amazing temporal, spatial and spectral resolution. Over the same period, the type and nature of numerical models in solar physics have been completely revolutionized as a result of widespread accessibility to parallel computers. These unprecedented advances on both observational and theoretical fronts have led to significant improvements in our understanding of many aspects of the Sun's behaviour and furthered our knowledge of plasma physics processes that govern solar and other astrophysical phenomena. In this Theme Issue, the current perspectives on the main astrophysical processes that shape our Sun are reviewed. In this Introduction, they are discussed briefly to help set the scene.

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The solar dynamo

Cited by 46 publications

References 84 publications

Flux Transport Dynamos: From Kinematics to Dynamics

Flux Transport Dynamos: From Kinematics to Dynamics

Magneto-convection

Astrophysical processes on the Sun

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