The Internal Solar Rotation in Its Spin-down History

Ruediger, G.; Kitchatinov, L. L.

doi:10.1086/177577

Cited by 55 publications

(55 citation statements)

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“…Thus, magnetic fields can potentially play a crucial role in the transport of momentum, chemical species, and magnetic flux on long and/or short time scales. In particular, on an evolutionary time scale, the tachocline may be considered as a boundary layer between the uniformly rotating radiative interior and differentially rotating convection zone with latitudinal variation (Rüdiger & Kitchatinov 1996;Gough & McIntyre 1998;MacGregor & Charbonneau 1999), and the dynamics of this boundary layer crucially depends on the values of the effective magnetic diffusivity, eddy viscosity, etc. The understanding of this boundary layer thus requires the prediction of these turbulent transport coefficients, derived from first principles.…”

Section: Introductionmentioning

confidence: 99%

On a long-term dynamics of the magnetised solar tachocline

Kim

Leprovost

2007

A&A

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Aims. We investigate the confinement and long-term dynamics of the magnetised solar tachocline. Methods. Starting from first principles, we derive the values of turbulent transport coefficients in the magnetised solar tachocline and then explore the implications for the confinement and long-term dynamics of the tachocline. Results. For reasonable parameter values, the turbulent eddy viscosity is found to be negative, with turbulence enhancing the radial shear in the tachocline. Both magnetic diffusivity and thermal diffusivity are severely quenched, with values much smaller than the magnitude of the eddy viscosity. The effect of the meridional circulation on momentum transport via the hyperviscosity becomes important when the radial shear becomes large (larger than the presently inferred value) due to negative viscosity. The results imply that the tachocline develops too strong radial shear to be a stationary Hartmann layer. In the limit of strong radiative damping where the turbulence is active on very small scales (<10 −4 R ), the eddy viscosity can become positive although its effect is likely to be dominated by the hyperviscosity. In comparison with the momentum transport, the transport of magnetic field, heat, and passive particles is more severely quenched. The results imply that the thickness of the tachocline is of order 10 −3 R −10 −2 R , independent of the strength of magnetic fields. In addition, the momentum transport is much more efficient than the particle mixing in the tachocline, consistent with the observations.

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Section: Introductionmentioning

confidence: 99%

On a long-term dynamics of the magnetised solar tachocline

Kim

Leprovost

2007

A&A

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“…Of course, there are other alternative mechanisms for maintaining thin tachocline. For instance, it may be through Lorentz force in the case of magnetized tachocline (Rüdiger & Kitchatinov 1996;Gough & McIntyre 1998;MacGregor & Charbonneau 1999). Nevertheless, the aforementioned positive feedback due to shearing can still play an important role in the overall dynamics of the tachocline and thus should be investigated.…”

Section: Discussionmentioning

confidence: 99%

Self-consistent theory of turbulent transport in the solar tachocline

Kim¹

2005

A&A

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Abstract.We present a self-consistent theory of turbulent transport in the solar tachocline by taking into account the effect of the radial differential rotation on turbulent transport. We show that the shearing by the radial differential rotation leads to reduction in turbulent transport of particles and momentum and the amplitude of turbulent flow via shear stabilization. The degree of reduction depends on the direction as well as the quantity that is transported. Specifically, particle transport in the vertical (radial) direction, orthogonal to the shear flow, is reduced with the scaling ∝A −2 while it is less reduced in the horizonal plane with the scaling ∝A −4/3 . Here, A is shearing rate, representing the radial differential rotation. A similar, but weaker, anisotropy also develops in the amplitude of turbulent flow. The results suggest that the radial differential rotation in the tachocline can cause anisotropy in turbulence intensity and particle transport with weaker turbulence in the radial direction even in the absence of density stratification and even when the turbulence is mainly driven radially by plumes from the convection zone. We also assess the efficiency of the transport by a meridional circulation by taking into account the interaction with the radial differential rotation. Implications for mixing and angular momentum transport in the solar interior is discussed.

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“…This approach has been used to model massive rotating stars over secular time scales (Palacios et al 2003;Meibom et al 2013) and to generate grids of stellar models used for isochrones and chemical evolution studies Georgy et al 2013;Lagarde et al 2012). Some attempts have also been made to model in 2-D the secular evolution of internal angular momentum by considering the role of large scale magnetic field in the radiative interior (see Charbonneau and MacGregor 1993;Ruediger and Kitchatinov 1996;Spada et al 2010, and references therein). However such models do not solve for dynamo action as we will now discuss in the next section.…”

Section: -D Stellar Evolution and Core-envelope Couplingmentioning

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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The Internal Solar Rotation in Its Spin-down History

Cited by 55 publications

References 0 publications

On a long-term dynamics of the magnetised solar tachocline

On a long-term dynamics of the magnetised solar tachocline

Self-consistent theory of turbulent transport in the solar tachocline

The Solar-Stellar Connection

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