Lecture 8 Double-diffusive convection

Slides:



Advertisements
Similar presentations
Cavitation and Bubble Dynamics Ch.2 Spherical Bubble Dynamics.
Advertisements

The example of Rayleigh-Benard convection. Pattern-forming instabilities: The example of Rayleigh-Benard convection.
Introduction Irina Surface layer and surface fluxes Anton
Thermal Instability “This seems such an economical and elegant method to make cloudy media, one feels that nature would be inexcusably remiss not to have.
Free Convection: Overview
Cumulus Forced; pushed upward by external forces, i.e. lifting by surface convergence, topography etc. Active; growing upward from self-forcing, i.e. buoyancy,
1 Hydrodynamic instabilities of autocatalytic reaction fronts: A. De Wit Unité de Chimie Physique non Linéaire Université Libre de Bruxelles, Belgium.
Plasma Astrophysics Chapter 7-1: Instabilities I Yosuke Mizuno Institute of Astronomy National Tsing-Hua University.
Lecture 3: Nocturnal (Stably Stratified) Boundary Layer.
Atmospheric Stability
Atmospheric Stability and Cloud Formation. RECAP Mechanical equilibrium: stable, unstable, neutral. Adiabatic expansion/compression: no heat exchange.
Cosmological Structure Formation A Short Course
Density Inversions in the Ocean Ben Kravitz. Potential Density Potential Density (ρ θ ) is the density a parcel of water would have if raised adiabatically.
Baroclinic Instability in the Denmark Strait Overflow and how it applies the material learned in this GFD course Emily Harrison James Mueller December.
Stellar Structure Section 4: Structure of Stars Lecture 7 – Stellar stability Convective instability Derivation of instability criterion … … in terms of.
Department of EECS University of California, Berkeley EECS 105 Fall 2003, Lecture 8 Lecture 8: Capacitors and PN Junctions Prof. Niknejad.
A k-  model for turbulently thermal convection in solar like and RGB stars Li Yan Yunnan Astronomical Observatory, CAS.
Analysis of the Rossler system Chiara Mocenni. Considering only the first two equations and ssuming small z The Rossler equations.
Lapse Rates and Stability of the Atmosphere
Review of Lecture 4 Forms of the radiative transfer equation Conditions of radiative equilibrium Gray atmospheres –Eddington Approximation Limb darkening.
Radiative Equilibrium
Probing the Reheating with Astrophysical Observations Jérôme Martin Institut d’Astrophysique de Paris (IAP) 1 [In collaboration with K. Jedamzik & M. Lemoine,
Physics of Convection " Motivation: Convection is the engine that turns heat into motion. " Examples from Meteorology, Oceanography and Solid Earth Geophysics.
Influences of Compositional Stratification S.E.Zaranek E.M. Parmentier Brown University Department of Geological Sciences.
Free Convection A free convection flow field is a self-sustained flow driven by the presence of a temperature gradient. (As opposed to a forced convection.
Supergranulation Waves in the Subsurface Shear Layer Cristina Green Alexander Kosovichev Stanford University.
BGU WISAP Spectral and Algebraic Instabilities in Thin Keplerian Disks: I – Linear Theory Edward Liverts Michael Mond Yuri Shtemler.
1 Flux Transport by Convection in Late-Type Stars (Mihalas 7.3) Schwarzschild Criterion Mixing Length Theory Convective Flux in Cool Star.
Ch 24 pages Lecture 10 – Ultracentrifugation/Sedimentation.
Lecture 19-20: Natural convection in a plane layer. Principles of linear theory of hydrodynamic stability 1 z x Governing equations: T=0T=0 T=AT=A h =1.
USE THESE VALUES. e(T) = e s (T Dew ) PRACTICE WITH STABILITY.
Summerschool Modelling of Mass and Energy Transport.
Models of the 5-Minute Oscillation & their Excitation Bob Stein – Michigan State U. 1.
Stability and Dynamics in Fabry-Perot cavities due to combined photothermal and radiation-pressure effects Francesco Marino 1, Maurizio De Rosa 2, Francesco.
Lecture Guidelines for GEOF110 Chapter 5 ( 2 hours) Chapter 6 (2 Hours) Ilker Fer Guiding for blackboard presentation. Following Pond & Pickard, Introductory.
Double diffusive mixing (thermohaline convection) 1. Semiconvection ( ⇋ diffusive convection) 2. saltfingering ( ⇋ thermohaline mixing) coincidences make.
HEAT TRANSFER FINITE ELEMENT FORMULATION
Ch 24 pages Lecture 11 – Equilibrium centrifugation.
Double Diffusion in the Core David Gubbins SEE, University of Leeds CIDER Community Workshop Marconi Center 2009 David Gubbins SEE, University of Leeds.
SOES6002 Module A, part 2: Multiple equilibria in the THC system: Governing equation Tim Henstock.
Definitions in-situ density anomaly: σs,t,p = ρ – 1000 kg/m3
Mecânica de Fluídos Ambiental 2015/2016
Analysis of the Rossler system Chiara Mocenni. Considering only the first two equations and assuming small z, we have: The Rossler equations.
Potential temperature In situ temperature is not a conservative property in the ocean. Changes in pressure do work on a fluid parcel and changes its internal.
ANGULAR MOMENTUM TRANSPORT BY MAGNETOHYDRODYNAMIC TURBULENCE Gordon Ogilvie University of Cambridge TACHOCLINE DYNAMICS
Cumulus Clouds. Instabilities Resulting in Vertical Overturning 1.Thermal Instability (Assuming uniform vertical pressure gradient) a) Static (Parcel.
ELIMINATION on a 3x3 1. Line up equations. 2. Perform “elimination” TWICE on the SAME variable using two DIFFERENT pairs of equations. 3. With the 2 equations.
Superconductivity and Superfluidity Landau Theory of Phase Transitions Lecture 5 As a reminder of Landau theory, take the example of a ferromagnetic to.
Relaminarisation of turbulent stratified flow Bas van de Wiel Moene, Steeneveld, Holtslag.
Heat Transfer Su Yongkang School of Mechanical Engineering # 1 HEAT TRANSFER CHAPTER 9 Free Convection.
Advanced Dynamical Meteorology Roger K. Smith CH 05.
Physics 313: Lecture 9 Monday, 9/22/08
Formation of universe, blackhole and 1st order phase transition
Two stable equilibria of the Atlantic subpolar gyre
Spectral and Algebraic Instabilities in Thin Keplerian Disks: I – Linear Theory Edward Liverts Michael Mond Yuri Shtemler.
Structural Design of Highway
thermal conductivity of a gas
Stability.
SCALING AND NON-DIMENSIONAL NUMBERS
Water Vapor Calculation
Modern Control Systems (MCS)
Eulerian vs Lagrangian
Stability and Cloud Development
Get out your reading guide from 15.2
Stability and Dynamics in Fabry-Perot cavities due to combined photothermal and radiation-pressure effects Francesco Marino1,4, Maurizio De Rosa2, Francesco.
Investigating Dansgaard-Oeschger events via a 2-D ocean model
Lecture 1: Introduction
Flux Transport by Convection in Late-Type Stars (Hubeny & Mihalas 16
Convection John Crooke 3/26/2019.
3rd Lecture : Integral Equations
Presentation transcript:

Lecture 8 Double-diffusive convection Discovered in oceanographic context Nowadays many applications Here: two diffusivities Thermal diffusivity acts destabilizing In astrophysics: semiconvection

Different diffusivities crucial kS=1.3 x 10-5 cm2 s-1 (sea water) kC=1.5 x 10-3 cm2 s-1 Le = kT/kC= Sc/Pr=Schmidt/Prandtl is large temperature in equilibrium, salinity not Diffusion can destabilize the system! not with single diffusing component

Two active scalars C for concentration of salinity Opposing trends: avoid S, which we used for entropy both aT>0 and aC>0 Opposing trends: if T increases, r decreases if C increases, r increases  Rayleigh-Benard-like problem

Origin in oceanography Stommel et al (1954) Stern (1960)

Case 1: more salt on top dT/dz>0 dC/dz>0 dr/dz<0 hot salty displacement hot salty blob lighter than surroundings blob heavier than surroundings fresh cold unstable stable unstable (top-heavy) but density stably stratified

Case 2: salt stabilizes unstable dT/dz dC/dz<0 dr/dz<0 displacement cold fresh blob heavier than surroundings blob lighter than surroundings salty hot “overstable” unstable Stable Stabilizing! again density stably stratified

Overstability? Originated from stellar stability   Hopf bifurcation (Gough 2003)  Hopf bifurcation

Boussinesq equations

Recall lecture 3, eq.(10) and (11) linearized, & double-curl Proceed analogously where

Reduce to single equation apply to both sides of and use on rhs

….to obtain Do simplest case: stress-free boundaries assume that principle of exchange of stabilities applicable

…works only for nonoscillatory onset But we see that that instability is possible if remember: Either negative T gradient big enough (i.e. 1st term dominant):  similar to Rayleigh-Benard convection but could be stabilized by negative C gradient or C gradient is positive and big enough (2nd term dominant): salt fingers

Dispersion relation substitute  Cubic equation Solve numerically Buoyancy frequencies  Cubic equation Solve numerically Onset, nonoscillatory (zero frequency) also: decaying, oscillatory modes (pair of finite frequencies)

Salt fingers

Dispersion relation: opposite case growing oscillatory modes (again pair of frequencies)

The two regimes

Staircase formation

Staircase formation Empirical fact, not from linear theory (nor weakly nonlinear theory)

Many applications! Oceanography Geology (magma chambers) Astrophysics Publications in double-diffusive Oceanography Geology (magma chambers) Astrophysics Engineering (metallurgy) Yet, not very highly thought of back in the 1950s

Astrophysical application: m-gradient Kato (1966)

In astrophysics: semi-convection  Lots of current research! Layered convection (Zaussinger & Spruit 2013)

Backup slides

x

x

x

x

x

“Salt fingers” in magma chamber

Comparison: the 2 regimes

Overstability?