double diffusive mixing (thermohaline convection)
DESCRIPTION
Double diffusive mixing (thermohaline convection) 1. Semiconvection ( ⇋ diffusive convection) 2. saltfingering ( ⇋ thermohaline mixing). coincidences make these doable. Density ( ) thermal diffusivity ( ), viscosity - PowerPoint PPT PresentationTRANSCRIPT
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Double diffusive mixing (thermohaline convection)
1. Semiconvection (⇋ diffusive convection)
2. saltfingering (⇋ thermohaline mixing)
coincidences make these doablecoincidences make these doable
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Density ( )
thermal diffusivity ( ), viscosity
solute (He) diffusivity
thermal overturning time
solute buoyancy frequency ( )
astro:
Prandtl number Lewis number (elsewhere denoted )
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‘saltfingering’, ‘thermohaline’S destabilizes, T stabilizes
‘diffusive’, ‘semiconvection’T destabilizes, S stabilizes
Double - diffusive convection: (RT-) stable density gradient
Two cases: ( , incompressible approx.)
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Both can be studied numerically, but only in a limited parameter range
W. MerryfieldF. Zaussinger
Saltfingeringsemiconvection
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Geophysical example: the East African volcanic lakes
Lake Kivu, (Ruanda ↔ DRC)
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Lake Kivu (Schmid et al 2010)
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double-diffusive ‘staircases’
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Linear stability (Kato 1966): predicts an oscillatory form of instability(‘overstability’)
↑displace up:(in pressure equilibrium)
cooling:
↑
gravity,temperature,solute
downward acceleration
⇓↑
Why a layered state instead of Kato-oscillations?
- physics: energy argument- applied math: ‘subcritical bifurcation’
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energy argument
Energy needed to overturn (adiabatically) a Ledoux-stable layer of thickness :
Per unit of mass:
vanishes as
: overturning in a stack of thin steps takes little energy.
sources:- from Kato oscillation,- from external noise (internal gravity waves from a nearby convection zone)
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Proctor 1981:
In the limit a finite amplitude layered state exists whenever the system in absence of the stabilizing solute is convectively unstable.
conditions:
(i.e. astrophysical conditions)
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‘weakly-nonlinear’ analysis of fluid instabilities
subcritical instability(semiconvection)
supercritical instability
(e.g. ordinary convection)
onset of linear instability: Kato oscillations
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← diffusion
← diffusion
← diffusion
convection
convection
layered convection:
diffusive interfacestable:
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semiconvection: 2 separate problems.
1. fluxes of heat and solute for a given layer thickness
2. layer thickness and its evolution
1: can be done with a parameter study of single layers
2: layer formation depends on initial conditions, evolution of thickness by merging: slow process, computationally much more demanding than 1.
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Calculations: a double-diffusive stack of thin layers
1. analytical model2. num. sims.
layers thin: local problem
symmetries of the hydro equations: parameter space limited
5 parameters:
: Boussinesq approx.
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Calculations: a double-diffusive stack of thin layers
1. analytical model2. num. sims.
layers thin: local problem
symmetries of the hydro equations: parameter space limited
5 parameters:
: Boussinesq approx.
limit : results independent of
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Calculations: a double-diffusive stack of thin layers
1. analytical model2. num. sims.
layers thin: local problem
symmetries of the hydro equations: parameter space limited
5 parameters:
: Boussinesq approx.
limit : results independent of
a 3-parameter space covers all
fluxes: + scalings to astrophysical variables
➙➙
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Fit to laboratory convection expts
Transport of S, T by diffusion
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boundary layers
flow overturning time
solute temperature - plume width
- solute contrast carried by plume is limited by net buoyancy
middle of stagnant zone
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Model (cf. Linden & Shirtcliffe 1978)
Stagnant zone: transport of S, T by diffusionOverturning zone:- heat flux: fit to laboratory convection- solute flux: width of plume , S-content given by buoyancy limit- stationary: S, T fluxes continuous between stagnant and overturning zone.- limit
➙ fluxes (Nusselt numbers):
astro: heat flux known, transform to
( )
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Heat flux held constant
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Model predicts existence of a critical density ratio
(cf. analysis Proctor 1981, Linden & Shirtcliffe 1978)
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Numerical (F. Zaussinger & HS, A&A 2013)
Grid of 2-D simulations to cover the 3-parameter space
- single layer, free-slip top & bottom BC, horizontally periodic, Boussinesq- double layer simulations- compressible comparison cases
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S T
Development from Kato oscillations
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Development of an interface
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Different initial conditions
Step
Linear
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Model predicts existence of a critical density ratio
(cf. analysis Proctor 1981, Linden & Shirtcliffe 1978)
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Wood, Garaud & Stellmach 2013:
Interpretation in terms of a turbulence model
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Wood, Garaud & Stellmach 2013:
fitting formula to numerical results:
(not extrapolated to astrophysical conditions)
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For astrophysical application:
valid in the range:
independent of
Semiconvective zone in a MS star (Weiss):
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Evolution of layer thickness(can reach ?)
merging processes
Estimate using the value of found- merging involves redistribution of solute between neighboring layers
layer thickness cannot be discussed independent of system history
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Conclusions
Semiconvection is a more astrophysically manageable process:
- thin layers local➙- small Prandtl number limit simplifies the physics- astrophysical case of known heat flux makes mixing rate independent of layer thickness- effective mixing rate only 100-1000 x microscopic diffusivity
mixing in saltfingering case (‘thermohaline’) is limitedby small scale of the process