The Rotation of the Deep Solar Layers

Couvidat, S.; García, R. A.; Turck‐Chièze, S.; Corbard, T.; Henney, C. J.; Jiménez-Reyes, S. J.

doi:10.1086/379698

Cited by 131 publications

(98 citation statements)

References 13 publications

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“…However, the same angular momentum transport model has failed to explain gamma-ray bursts (Woosley & Heger 2004). Finally, Eggenberger et al (2005) have recently demonstrated that the Tayler-Spruit dynamo leads to a nearly flat solar rotation profile consistent with that revealed by the helioseismic data (e.g., Couvidat et al 2003). The important question of stellar spin-down was not directly addressed in this theoretical work.…”

Section: Introductionmentioning

confidence: 87%

“…Our results are summarized in Figure 3. In Figure 3b, we compare the normalized solar rotation as a function of radius obtained from the helioseismic data of Couvidat et al (2003; dots with error bars) to a model without angular momentum transport (long-dashed line), a full evolutionary model using the Maeder & Meynet (2004) prescription (solid line), and rotation curves derived from static models with -profiles appropriate for solar models at ages of 150 and 600 Myr, and 4.57 Gyr (dotted, shortdashed, and dot-dashed lines, respectively). In Figure 3a, we compare the magnetic viscosities that we would have obtained for the no-transport rotation curve using our prescription (solid line) and the Maeder & Meynet (2004) prescription (dashed line).…”

Section: Comparison With Observationsmentioning

confidence: 99%

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A Revised Prescription for the Tayler‐Spruit Dynamo: Magnetic Angular Momentum Transport in Stars

Denissenkov

Pinsonneault

2007

ApJ

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Angular momentum transport by internal magnetic fields is an important ingredient for stellar interior models. In this paper we critically examine the basic heuristic assumptions in the model of the Tayler-Spruit dynamo, which describes how a pinch-type instability of a toroidal magnetic field in differentially rotating stellar radiative zones may result in large-scale fluid motion. We agree with prior published work both on the existence of the instability and its nearly horizontal geometry for perturbations. However, the approximations in the original Acheson dispersion relation are valid only for small length scales, and we disagree that the dispersion relation can be extrapolated to horizontal length scales of order the radius of the star. We contend that dynamical effects, in particular, angular momentum conservation, limit the maximum horizontal length scale. We therefore present transport coefficients for chemical mixing and angular momentum redistribution by magnetic torques that are significantly different from previous published values. The new magnetic viscosity is reduced by 2-3 orders of magnitude compared to the old one, and we find that magnetic angular momentum transport by this mechanism is very sensitive to gradients in the mean molecular weight. The revised coefficients are more compatible with empirical constraints on the timescale of core-envelope coupling in young stars than the previous ones. However, solar models including only this mechanism possess a rapidly rotating core, in contradiction with helioseismic data. Previous studies had found strong core-envelope coupling, both for solar models and for the cores of massive evolved stars. We conclude that the Tayler-Spruit mechanism may be important for envelope angular momentum transport but that some other process must be responsible for efficient spin-down of stellar cores.

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Section: Introductionmentioning

confidence: 87%

Section: Comparison With Observationsmentioning

confidence: 99%

A Revised Prescription for the Tayler‐Spruit Dynamo: Magnetic Angular Momentum Transport in Stars

Denissenkov

Pinsonneault

2007

ApJ

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“…In addition to observations of stellar surface properties, those of the solar five-minute oscillations have provided a wealth of information on the internal structure of the Sun and have led Article published by EDP Sciences L4, page 1 of 4 to the determination of its rotation profile (Brown et al 1989;Elsworth et al 1995;Kosovichev et al 1997;Couvidat et al 2003;García et al 2007). This major constraint on the modelling of angular momentum transport shows that rotating models including meridional circulation and shear turbulence are unable to reproduce the near uniformity of the solar rotation profile (Pinsonneault et al 1989;Chaboyer et al 1995;Eggenberger et al 2005;Turck-Chièze et al 2010).…”

Section: Introductionmentioning

confidence: 99%

Angular momentum transport in stellar interiors constrained by rotational splittings of mixed modes in red giants

Eggenberger

Montalbán

Miglio

2012

A&A

218

254

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Context. Recent asteroseismic observations have led to the determination of rotational frequency splittings for ℓ = 1 mixed modes in red giants. Aims. We investigate how these observed splittings can constrain the modelling of the physical processes transporting angular momentum in stellar interiors. Methods. We first compare models including a comprehensive treatment of shellular rotation only, with the rotational splittings observed for the red giant KIC 8366239. We then study how these asteroseismic constraints can give us information about the efficiency of an additional mechanism for the internal transport of angular momentum. This is done by computing rotating models of KIC 8366239 that include a constant viscosity corresponding to this physical process, in addition to the treatment of shellular rotation. Results. We find that models of red giant stars including shellular rotation only predict steep rotation profiles, which are incompatible with the measurements of rotational splittings in the red giant KIC 8366239. Meridional circulation and shear mixing alone are found to produce an insufficient internal coupling so that an additional mechanism for the internal transport of angular momentum is needed during the post-main sequence evolution. We show that the viscosity ν add corresponding to this mechanism is strongly constrained to be ν add = 3 × 10 4 cm 2 s −1 thanks to the observed ratio of the splittings for modes in the wings to those at the centre of the dipole forests. Such a value of viscosity may suggest that the same unknown physical process is at work during the main sequence and the post-main sequence evolution.

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“…Thompson et al 1996) and the radiative zone (e.g. Chaplin et al 1999a;Couvidat et al 2003;Eff-Darwich et al 2008;Eff-Darwich & Korzennik 2013;Elsworth et al 1995;García et al 2004García et al , 2008c or the conditions and properties of the solar core (e.g. Appourchaux et al 2010;Basu et al 1997Basu et al , 2009García et al 2007García et al , 2008aTurck-Chièze et al 2001, 2004 are some wellknown examples.…”

Section: Helio and Asteroseismologymentioning

confidence: 99%

Observational techniques to measure solar and stellar oscillations

García

2015

EAS Publications Series

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Abstract.As said by Sir A. Eddington in 1925: "Our telescopes may probe farther and farther into the depths of space. At first sight it would seem that the deep interior of the sun and stars is less accessible to scientific investigation than any other region of the universe. What appliance can pierce through the outer layers of a star and test the conditions within?" Eddington (1926). Nowadays, asteroseismology has proven its ability to pierce below stellar photospheres and allow us to "see" inside the interior of thousands of stars down to the stellar cores, answering the question asked by Eddington ninety years ago. In this chapter we review the general properties of the spectral analysis which is the base of any asteroseismic investigation. After describing the stellar power spectrum, we will describe in details the characterization of the modal spectrum. This chapter will end by a brief description of the instrumentation in both helio and asteroseismology.

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The Rotation of the Deep Solar Layers

Cited by 131 publications

References 13 publications

A Revised Prescription for the Tayler‐Spruit Dynamo: Magnetic Angular Momentum Transport in Stars

A Revised Prescription for the Tayler‐Spruit Dynamo: Magnetic Angular Momentum Transport in Stars

Angular momentum transport in stellar interiors constrained by rotational splittings of mixed modes in red giants

Observational techniques to measure solar and stellar oscillations

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