ERRATUM: “TURBULENT MIXING AND LAYER FORMATION IN DOUBLE-DIFFUSIVE CONVECTION: THREE-DIMENSIONAL NUMERICAL SIMULATIONS AND THEORY” (2011, ApJ, 731, 66)

Rosenblum, Erica; Garaud, Pascale; Traxler, Adrienne L.; Stellmach, Stephan

doi:10.1088/0004-637x/742/2/132

Cited by 19 publications

(54 citation statements)

References 1 publication

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“…This mechanism, known as the γ−instability, was originally put forward by Radko (2003) to explain layer formation in fingering convection but was found to apply to ODDC as well. The simulations of Rosenblum et al (2011) also demonstrated the existence of a non-layered phase of ODDC which had been neglected by nearly all previous studies except that of Langer et al (1985), who proposed a model for mixing of chemical species by semiconvection that ignores layering entirely (see reviews by Merryfield 1995;Moll et al 2016). Next, Mirouh et al (2012) identified the parameter regimes in which layers do and do not form by the γ−instability in ODDC.…”

Section: Introductionmentioning

confidence: 73%

“…Advances in high-performance computing have made it feasible to study ODDC using 3D numerical simulations. Rosenblum et al (2011) discovered that layers may form spontaneously in a linearly unstable system, and proposed a mechanism to explain how layer formation occurs. This mechanism, known as the γ−instability, was originally put forward by Radko (2003) to explain layer formation in fingering convection but was found to apply to ODDC as well.…”

Section: Introductionmentioning

confidence: 99%

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The Effect of Rotation on Oscillatory Double-Diffusive Convection (Semiconvection)

Moll

Garaud

2016

ApJ

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Oscillatory double-diffusive convection (ODDC, more traditionally called semiconvection) is a form of linear double-diffusive instability that occurs in fluids that are unstably stratified in temperature (Schwarzschild unstable), but stably stratified in chemical composition (Ledoux stable). This scenario is thought to be quite common in the interiors of stars and giant planets, and understanding the transport of heat and chemical species by ODDC is of great importance to stellar and planetary evolution models. Fluids unstable to ODDC have a tendency to form convective thermo-compositional layers which significantly enhance the fluxes of temperature and chemical composition compared with microscopic diffusion. Although a number of recent studies have focused on studying properties of both layered and non-layered ODDC, few have addressed how additional physical processes such as global rotation affect its dynamics. In this work we study first how rotation affects the linear stability properties of rotating ODDC. Using direct numerical simulations we then analyze the effect of rotation on properties of layered and non-layered ODDC, and study how the angle of the rotation axis with respect to the direction of gravity affects layering. We find that rotating systems can be broadly grouped into two categories, based on the strength of rotation. Qualitative behavior in the more weakly rotating group is similar to non-rotating ODDC, but strongly rotating systems become dominated by vortices that are invariant in the direction of the rotation vector and strongly influence transport. We find that whenever layers form, rotation always acts to reduce thermal and compositional transport.

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Section: Introductionmentioning

confidence: 73%

Section: Introductionmentioning

confidence: 99%

The Effect of Rotation on Oscillatory Double-Diffusive Convection (Semiconvection)

Moll

Garaud

2016

ApJ

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“…DDC can occur in regions that are found to be stable against convection according to the Ledoux criterion, but unstable according to Schwarzschild criterion (Rosenblum et al 2011;Wood et al 2013). In these regions, the heat transport rate in our model is lower than in the case of DDC, since we treat these regions as being radiative/conductive.…”

Section: Double-diffusion Convectionmentioning

confidence: 99%

Jupiter’s evolution with primordial composition gradients

Vazan

Helled

Guillot

2018

A&A

106

128

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Recent formation and structure models of Jupiter suggest that the planet can have composition gradients and not be fully convective (adiabatic). This possibility directly affects our understanding of Jupiter's bulk composition and origin. In this Letter we present Jupiter's evolution with a primordial structure consisting of a relatively steep heavy-element gradient of 40 M ⊕ . We show that for a primordial structure with composition gradients, most of the mixing occurs in the outer part of the gradient during the early evolution (several 10 7 years), leading to an adiabatic outer envelope (60% of Jupiter's mass). We find that the composition gradient in the deep interior persists, suggesting that ∼40% of Jupiter's mass can be non-adiabatic with a higher temperature than the one derived from Jupiter's atmospheric properties. The region that can potentially develop layered-convection in Jupiter today is estimated to be limited to ∼10% of the mass.

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“…The value of α is still discussed in the literature by hydrodynamic simulations in 2D or 3D (Denissenkov et al 2009;Denissenkov 2010;Denissenkov & Merryfield 2011;Rosenblum et al 2011;Traxler et al 2011;Brown et al 2013;Garaud & Brummell 2015). Although these simulations are still far from stellar conditions and do not take into account the coupling of this instability with other hydrodynamic processes occurring in red giant stars (e.g.…”

Section: Physicsmentioning

confidence: 99%

TheGaia-ESO Survey: impact of extra mixing on C and N abundances of giant stars

Lagarde

Reylé

Robin

et al. 2018

A&A

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Context. The Gaia-ESO Public Spectroscopic Survey using FLAMES at the VLT has obtained high-resolution UVES spectra for a large number of giant stars, allowing a determination of the abundances of the key chemical elements carbon and nitrogen at their surface. The surface abundances of these chemical species are known to change in stars during their evolution on the red giant branch (RGB) after the first dredge-up episode, as a result of the extra mixing phenomena. Aims. We investigate the effects of thermohaline mixing on C and N abundances using the first comparison between the Gaia-ESO survey [C/N] determinations with simulations of the observed fields using a model of stellar population synthesis. Methods. We explore the effects of thermohaline mixing on the chemical properties of giants through stellar evolutionary models computed with the stellar evolution code STAREVOL. We include these stellar evolution models in the Besançon Galaxy model to simulate the [C/N] distributions determined from the UVES spectra of the Gaia-ESO survey and to compare them with the observations.Results. Theoretical predictions including the effect of thermohaline mixing are in good agreement with the observations. However, the field stars in the Gaia-ESO survey with C and N abundance measurements have a metallicity close to solar, where the efficiency of thermohaline mixing is not very large. The C and N abundances derived by the Gaia-ESO survey in open and globular clusters clearly show the impact of thermohaline mixing at low metallicity, which explains the [C/N] value observed in lower mass and older giant stars. Using independent observations of carbon isotopic ratio in clump field stars and open clusters, we also confirm that thermohaline mixing should be taken into account to explain the behaviour of 12 C/ 13 C as a function of stellar age. Conclusions. Overall, the current model including thermohaline mixing is able to reproduce very well the C and N abundances over the whole metallicity range investigated by the Gaia-ESO survey data.

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ERRATUM: “TURBULENT MIXING AND LAYER FORMATION IN DOUBLE-DIFFUSIVE CONVECTION: THREE-DIMENSIONAL NUMERICAL SIMULATIONS AND THEORY” (2011, ApJ, 731, 66)

Cited by 19 publications

References 1 publication

The Effect of Rotation on Oscillatory Double-Diffusive Convection (Semiconvection)

The Effect of Rotation on Oscillatory Double-Diffusive Convection (Semiconvection)

Jupiter’s evolution with primordial composition gradients

TheGaia-ESO Survey: impact of extra mixing on C and N abundances of giant stars

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