Dynamo Models of the Solar Cycle

Charbonneau, Paul

doi:10.12942/lrsp-2010-3

Cited by 656 publications

(522 citation statements)

References 266 publications

(264 reference statements)

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“…We refer to the papers by Küker et al (2001), Käpylä et al (2006) and the reviews by Fisher et al (2000); Tobias (2002);Ossendrijver (2003); Charbonneau (2010); de Jager and Duhau (2011);Schmieder et al (2014);Fletcher et al (2015). Many more papers could be mentioned but we do not consider that necessary because a treatment of dynamo theories is outside the scope and purposes of the present paper.…”

Section: The Tachocline; the Origin Of Sunspotsmentioning

confidence: 99%

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A Remarkable Recent Transition in the Solar Dynamo

et al. 2016

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We summarize the major aspects of the remarkable, fairly long lasting period (∼ 2005 to ∼ 2010) of low solar activity, that we will call the Transition. It is the transitional stage between the Grand Maximum of the 20th century and a forthcoming (most probably Regular) episode of solar activity. The various kinds of activity in the functioning of the equatorial components of the solar dynamo before and during the Transition are summarized. While the behavior of unipolar magnetic regions and their rest-latitudes already gave very early indications -mid 20th century -of the forthcoming Transition, more such indications became available around 1995 and the main part of it occurred between 2005 and 2010. Some of the inferences are discussed. We submit the hypothesis that the solar tachocline undergoes pulsations and we present some helioseismic evidences. In that scenario we find that its equatorial part has moved downward over a fairly small semi-amplitude (∼ 0.03 solar radii) during the time of the Transition. There are several indications, apart from this 'pulsation', that the tachocline may even be pulsating with still smaller amplitudes in more modes. We speculate about the physical mechanism(s).

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Section: The Tachocline; the Origin Of Sunspotsmentioning

confidence: 99%

“…Another viewpoint may be that the tachocline, as observed by helioseismology, is undergoing a differential rotation with respect to the solar core that leads to torsional oscillation of the whole convective layer (cf. Charbonneau 2010). In that line, wrote ".…”

Section: Pulsations?mentioning

confidence: 99%

A Remarkable Recent Transition in the Solar Dynamo

et al. 2016

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“…From our analysis of MDI and Wilcox magnetogram data we have looked in particular at the axisymmetric modes from = 1 to 6, since these are the ones most easily compared with the output from 2-D mean field dynamo models. When comparing standard flux transport dynamo models (Jouve & Brun 2007, Charbonneau 2010, Choudhuri 2012) with solar observations it was noticed that in such models the secondary family is not excited and does not maintain a level similar to that seen on the Sun (DBH12). This is expected from the equatorial symmetry of the flow profiles and poloidal source terms used in most mean field dynamo models (see GZ93, McFadden et al 2011, DBH12).…”

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confidence: 99%

On the role of asymmetries in the reversal of the solar magnetic field

Brun¹,

DeRosa

Hoeksema

2012

Proc. IAU

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Abstract. We study how the solar magnetic field evolves from antisymmetric (dipolar) to symmetric (quadrupolar) state during the course of its 11-yr cycle. We show that based on equatorial symmetries of the induction equation, flux transport solar mean field dynamo models excite mostly the antisymmetric (dipolar) family whereas a decomposition of the solar magnetic field data reveals that both families should be excited to similar amplitude levels. We propose an alternative solar dynamo solution based on North-South asymmetry of the meridional circulation to better reconcile models and observations.

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“…Moffatt 1978;Charbonneau 2010). The generated magnetic fields are manifested at the surface through starspots or polar caps, and contribute to the dynamic activity of the star.…”

Section: Solar Dynamics and Magnetism In A Stellar Contextmentioning

confidence: 99%

The Solar-Stellar Connection

Brun¹,

García²,

Houdek³

et al. 2017

Space Sciences Series of ISSI

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We discuss how recent advances in observations, theory and numerical simulations have allowed the stellar community to progress in its understanding of stellar convection, rotation and magnetism and to assess the degree to which the Sun and other stars share similar dynamical properties. Ensemble asteroseismology has become a reality with the advent of large time domain studies, especially from space missions. This new capability has provided improved constraints on stellar rotation and activity, over and above that obtained via traditional techniques such as spectropolarimetry or CaII H&K observations. New data and surveys covering large mass and age ranges have provided a wide parameter space to confront theories of stellar magnetism. These new empirical databases are complemented by theoretical advances and improved multi-D simulations of stellar dynamos. We trace these pathways through which a lucid and more detailed picture of magnetohydrodynamics of solar-like stars is beginning to emerge and discuss future prospects.

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Dynamo Models of the Solar Cycle

Cited by 656 publications

References 266 publications

A Remarkable Recent Transition in the Solar Dynamo

A Remarkable Recent Transition in the Solar Dynamo

On the role of asymmetries in the reversal of the solar magnetic field

The Solar-Stellar Connection

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