Planetary Waves in Planetary and Stellar Atmospheres › ... › 2008_Walterscheid.pdfObservational...
Transcript of Planetary Waves in Planetary and Stellar Atmospheres › ... › 2008_Walterscheid.pdfObservational...
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Waves in Planetary Atmospheres
R. L. Walterscheid
©2008 The Aerospace Corporation
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The Wave Zoo
Lighthill, Comm. Pure Appl. Math., 20, 1967
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Wave-Deformed Antarctic Vortex
Courtesy of VORCORE Project, Vial et al., 2007
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Atmospheric Waves
• Some waves that are common to rotating bodies with sensible atmospheres
– Rossby-Haurwitz– Gravity– Tides– Kelvin– Acoustic– Inertial
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Large-Scale Waves
• Here I focus on two broad classes of large-scale waves
• Planetary (Rossby-Haurwitz) waves– “Planetary” refers to both the scale of the wave
and to dynamics peculiar to rotating bodies– Planetary waves are waves that depend in some
way on the effects of rotation – in particular on the variation of the vertical component of rotation with latitude
• Gravity waves– Wave in a stratified medium and for which gravity
is the restoring force• Atmospheric tides include both classes
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Components of Motion
Lighthill, Comm. Pure Appl. Math., 20, 1967
Gravity Waves
Rossby Waves
Diverg-ence
Vortic-ity
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Observational IntroductionTraveling Free Waves
Eliasen and Machenhauer, 1965 (Tellus, 17, p 220-238)
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Observational IntroductionStationary Waves
Charney, Dynamic
Meteorology, D. Reidel,
1973
500 hPa
10 hPa
Summer Winter
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Observational IntroductionGravity Waves
Image courtesy NASA/GSFC/LaRC/JPL,MISR Team
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Observational IntroductionAtmospheric Tides
Nastrom and Belmont, J. Atmos. Sci., 1976
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Dynamics of Planetary WavesVorticity
• Vorticity
– Curl of velocity
– Mainly interested in vertical component
– For a body in solid rotation
• Absolute vorticity
– Sum of relative vorticity and planetary vorticity
Ω= 2ς
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Planetary WavesMechanism for Wave Motion (1)
) vorticity(relative ) vorticity(planetary sin2
constant ~ vorticityabsolute
yuxvf
f
∂∂−∂∂=Ω=
=+
ςϕ
ς
funtion Stream ˆ
=
∇×−=
ψ
ψψ ku
ψς 2∇=
⇒Vorticity a function of curvature along stream line
Rotational part of wind field
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Planetary WavesMechanism for Wave Motion (2)
y(N) f
x(E)
f increasingdecreasingς
f decreasingincreasingς
Restoring mechanism is latitudinal gradient of planetary vorticity
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Propagation of Rossby WavesMechanism of Wave Propagation
++dydf-
Vorticity tendency due to advection of planetary vorticity induces westward motion
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Prototype Rossby Waves• Non-divergent barotropic motion on a β-plane
• Dispersion relation
• Phase velocity
• Group velocity
kβω −=
( )( ) constant 0
00
=∂∂=−+=yf
yyffβ
β
(westward) 2kc β−=
(eastward) 2kug β+=
cug −=
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Rossby Wave Group PropagationHovmöller Diagram
Martius et al., Tellus, 2006
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Dynamics of Gravity Waves
• Exist in stratified fluids in gravitational fields
• Propagate horizontal divergence
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Gravity Waves
Wave propagates through interplay between horizontal divergence and pressure gradients in a
gravitational field
h
η
0>′p
X
Z
ρηgp =′
0=′p 0=′p
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Prototype Gravity Waves
22 khg=ω
• Dispersion relation for waves in shallow water ( )
Wave motion of an irrotational nondivergent fluid with a free surface
• Phase speed
hgcx ±=
xg cu =
• Group speed
hlx >>
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Quantitative Theory of Oscillations on a Rotating Sphere
Oscillations of an Ideal Ocean
• Oscillations of the free surface of an ocean of uniform undisturbed depth covering a rotating planet
• Shallow water equations
– Shallow compared to horizontal scale of the motion
– Quasi-static
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Quantitative Theory of Oscillations on a Rotating Sphere
• Laplace’s Tidal Equations– Linearized equations for motions on a
background state of rest– Describes a variety of wave types
• Rossby-Haurwitz waves• Gravity waves• Kelvin• Tides
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Laplace’s Tidal Equations for an Ideal Ocean
( )
( )
( ) (3) 01coscos1
(2) sin2
(1) cos
sin2
=∂
′∂+⎥
⎦
⎤⎢⎣
⎡∂
′∂+
∂′∂
∂′∂
−=′Ω+∂
′∂∂
′∂−=′Ω−
∂′∂
thgvu
a
au
tv
av
tu
φϕϕ
λϕ
ϕφϕ
λϕφϕ
surface free theofHeight =−=
hhhη
ηφλϕ
gLongitude Latitude
=′==
ϕλϕ
ψψψ
&
&
avau
==
−=′
cos raterotation Planetary radiusPlanetary
=Ω=a
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Waveform Solutions
Assume solutions of the form
( ) ( ) ( )[ ]λωϕλϕφ stit −Φ=′ exp,,
frequency Waver Wavenumbe Zonal
==
ωs
where
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Laplace’s Tidal Equation
( )[ ] ( )ϕεϕ ωω ssF ,, Θ=Θ
( )raterotation angular Planetary
2frequency onalNondemensi parameter Lambs
radiusPlanetary sin
=ΩΩ==
===
ωε
ϕμ
f
a
where
⎥⎦
⎤⎢⎣
⎡
−+⎟⎟
⎠
⎞⎜⎜⎝
⎛−+
−−⎟⎟
⎠
⎞⎜⎜⎝
⎛−
−= 222
22
2222
2
111
μμμ
μμμμ
μs
ff
fs
fdd
fddF
( )hga 22Ω
=ε
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Eigensolutions
• Eigenvalues– f (eigenfrequency)
• Eigenfunction – Hough Functions
• Solutions depend parametrically on s and ε– For every s and ε there is a complete set of modes
each with a different frequency
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Oscillations on a SphereWave Types (Limiting Cases)
• Small εf– Large Class 1 (Irrotational gravity waves
on a sphere)
• Eastward and westward propagation
– Small Class 2 (Nondivergent Rossby-Haurwitz waves)
• Propagate only westward
⇒f
⇒f
( ) ( ) ( )μμε sn
snn Pnnf =Θ+= 12
( ) ( ) ( )μμ sn
snn P
nnsf =Θ+
−=1
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EigensolutionsEigenfrequencies
Longuet-Higgins, Trans. Roy. Soc. London, Ser. A, 1968
f
ε−1/2
MRG
Rossby Waves
Gravity Waves
Gravity Waves
MRG
Kelvin Wave
EastwardWestward
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EigensolutionsEigenfunctions
Longuet-Higgins, Trans. Roy. Soc. London, Ser. A, 1968
ε
NP
Eq
ϕ-90
°
Θ(ϕ-90°)
As increases the eigenfunctions become
increasingly equatorially trapped
ε
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Tidal Equations for an Atmosphere
( )
( )
( ) ( ) (4) 0coscos1
(3) 0
(2) sin2
(1) cos
sin2
=∂′∂
+⎥⎦
⎤⎢⎣
⎡∂
′∂+
∂′∂
=′+∂
′∂∂
′∂−=′Ω+
∂′∂
∂′∂
−=′Ω−∂
′∂
−
zewvu
a
wSt
au
tv
av
tu
z
z
ϕϕ
λϕ
φϕ
φϕ
λϕφϕ
( )
surface constant ofHeight
g
log 0
zhhh
zwppz
=−=
=′==
η
ηφ&
( )
zeTgTRH
dzdHgzS
κθ
θ
=
=
=log
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Traveling Oscillations in an Atmosphere
Assume solutions of the form
( ) ( ) ( )[ ]λωϕλϕ stizWtzw −=′ exp,,,,
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Traveling Oscillations in an AtmospherePDE for Oscillations on a Motionless
Background State
Separable in height and latitude
( ) ( ) ( )[ ] 0,4
,1 22 =Ω
+∂∂
⎥⎦⎤
⎢⎣⎡ −∂∂ zWF
azSzW
zzϕϕ
( ) ( ) ( )ϕθϕ zwzW ˆ, =
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Traveling Oscillations in an AtmosphereSeparation of Variables
Vertical structure equation
( ) ( ) ( ) 0ˆˆ1 =+⎥⎦⎤
⎢⎣⎡ − zw
ghzSzw
dzd
dzd
( )[ ] ( )ϕεϕ Θ=ΘF
Horizontal structure equation
Equivalent depth (separation constant)
gah /)2( 2εΩ=
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Refractive Index for Vertical Propagation
( ) ( ) ( ) 0~~ 22
2
=+ zwzmzwdzd
( )412 −=
ghzSm
( ) ( ) ( )2expˆ~ zzwzw −=
The vertical structure equation can be placed in canonical form by transforming the dependent variables
( )imzBimzAwm −+=⇒> exp)exp(~02
( )zmBzmAwm 222 exp)exp(~0 −++=⇒<
For m2 constant
2
22
41Hgh
Nm −=
Dimensionally
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Vertical Structure• Waves in a continuously stratified fluid (atmospheres)
may be internal or external– Internal waves exhibit wave-like behavior in the
vertical direction• Transfer energy vertically• Conservative waves maintain nearly constant energy
density with altitude• Implies that wave amplitude grows exponentially with
altitude • Small amplitude waves originating in the lower
atmosphere may achieve large amplitudes in the upper atmosphere
– External waves have constant phase with height• Wave amplitude decays in height (evanescent)
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Traveling Oscillations in an AtmosphereMethod of Solution
• Find eigensolution of VSE →
– Vertical structure
– Equivalent depth h
• Find eigensolutions of HSE →
– Eigenfunctions
– Eigenfrequencies ω
( )ϕθ
( )zw′
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EigensolutionsEigenfrequencies
Longuet-Higgins, Trans. Roy. Soc. London, Ser. A, 1968
f
ε−1/2
Rossby Waves
h=γH
5-days
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Traveling Oscillations in an AtmosphereLamb Waves
• For the terrestrial atmosphere there is only one eigensolution for the VSE
– Lamb waves (waves for which the vertical velocity is identically zero)• Propagate horizontally as pure compression waves
– Vertical structure is evanescent• Wave amplitude
• Combined solutions (vertical + horizontal) are Lamb-Rossby waves
[ ]zκexp∝
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Traveling Oscillations in an AtmosphereSources
• Free waves are easy to excite and maintain
• May be excited by
– Selective response to random fluctuations
– Wave-wave interactions
– Parametric instabilities
• Main free waves in the terrestrial atmosphere
– 2, 5 and 16 day waves
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Traveling Oscillations in an AtmosphereThe 5-Day Wave (Latitude-Height Structure)
Hirooka, J. Atmos. Sci., 2000
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Traveling Oscillations in an AtmosphereThe 5-Day Wave (Vertical Structure)
Hirooka, J. Atmos. Sci., 2000
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Forced Waves
• May have internal wave structure• The forcing determines the frequency
– Rather than one equivalent depth associated with many frequencies there are many equivalent depths associated with a given frequency
– Equivalent depths found from HSE– Vertical structure depends on h as a
parameter
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Forced SolutionsTides
Longuet-Higgins, Trans. Roy. Soc. London, Ser. A, 1968
f
ε−1/2
Diurnal s=1 Tide
For forced waves negative equivalent depths are also
possible
gah /)2( 2εΩ=
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Waves on Other Planets
• Wave features are seen in the permanent cloud cover surrounding Venus
– Kelvin waves
– Rossby waves
• Planetary wave features are also seen in the atmosphere of Jupiter
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Waves in the Venus AtmosphereSm
ith e
t al.,
J.
Atm
os. S
ci.,
1993
Courtesy of G. Schubert
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Stationary Waves
• Quasi-geostrophic dynamics
• Vertical propagation
– Charney-Drazin theory
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Stationary WavesQuasi-Geostrophic Dynamics
• Motion nondivergent except when coupled to planetary vorticity
• Stream function is geostrophic
• Dynamics governed by quasi-geostrophic potential vorticity equation
– Potential vorticity includes the effects of divergence on vorticity change (conserved for barotropic divergent flow)
• Linearized quasi-geostrophic potential vorticity equation governs propagation of extratropical waves through zonal mean flows
fϕψ =
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Stationary WavesVertical Propagation (Charney-Drazin Theory)
Vertical Wavenumber for constant background winds
For m2 <0 waves attenuate with altitude
For c=0 (stationary waves)
Only long waves can propagate through strong winter westerlies
No waves can propagate through summer easterlies
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Stationary WavesSources
• Excited mainly by flow over large continental mountain areas
• Stronger in the northern hemisphere
• Strongest waves are the very long waves (s=1-3)
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Wave Transports• Transports originate in the nonlinear advective
(convective) terms
...
,
+′′⋅−∇=∂∂
→′+=′+=
AtA
AAA
u
uuu
ρρ
flux Wave=′′Auρ
...+⋅∇−=∂∂ AtA uρρ
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Wave Transports• Planetary waves transport heat momentum and
constituents (e.g., ozone) latitudinally• They play an significant role in the heat,
momentum and ozone budgets• The transports may force changes (sometimes
dramatic) in the mean state when waves are– Transient– Nonconservative– Nonlinear– Encounter a critical level
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TransportsRole in sudden Stratospheric Warmings
• Sudden Warmings are forced by a sudden amplification of stationary waves in the high latitude winter stratosphere
• Decelerates polar westerlies and waves transport heat northward
• Circumpolar vortex breaks down and winds change from westerlies to easterlies
• Warming near the pole can exceed 50K in the stratosphere
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Sudden Stratospheric Warming
Andrews et al., Middle Atmosphere Dynamics, 1987
Feb 17
Feb 21
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The Coldest Place in the Earth’s Atmosphere is the Summer Polar Mesopause
Effect of Dissipating Waves
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Deceleration of the Stratospheric Jets• Wave drag decelerates the stratospheric
winds
• Dominant contributor is thought to be small-scale gravity waves
• Causes the jets to close
• Cooling over summer pole is implied by thermal wind relation
yfTR
zu
∂∂
−=∂∂
Positive shear (decreasing westward winds) implies colder temperatures to the
north
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Waves in the Ionosphere-Thermosphere System
• Tides– Periodic response to astronomical forcing– Diurnal period and its harmonics (principally
semidiurnal)– Forced by absorption of solar radiation by
atmospheric constituents (O3, H2O, O2, …)– Lower thermosphere diurnal variation
dominated by tides forced in troposphere and stratosphere
– Middle and upper thermosphere dominated by tides forced in situ
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Waves in the I-T System (Cont.)
• Gravity waves
– Excited in lower atmosphere and auroral zone
• Traveling Planetary waves
– Upward extensions of waves in mesosphere
– Possibly excited by geomagnetic storms
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Tides in Lower Thermosphere
Burrage et al., GRL, 1995
Daily estimates of diurnal tidal amplitude from HRDI data for an
altitude of 95 km
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Planetary Waves in the IonosphereTwo-Day-Wave
Pancheva, JGR, 2006
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Gravity Waves in the I-T
Traveling Atmospheric Disturbances seen in density near 400 km measured by the accelerometer on the CHAMP satellite in connection with a geomagnetic disturbance. The disturbances appear to penetrate into opposite hemispheres from their origins.
Forbes, J. Met. Soc. Japan, 2007
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Summary• Traveling free waves are normal modes of Laplace’s
Tidal Equation• Free traveling planetary waves are prominent features of
the stratosphere• Quasi-stationary waves dominate mid-latitude long-wave
field during winter– Transport heat, momentum and ozone– Induce large changes in the mean state
• Sudden mid-winter Stratospheric Warmings• Maintain summer polar mesopause out of radiative
equilibrium• Long-term (semi-annual, quasi-biennial) oscillations
• Waves in the I-T system achieve large amplitudes and respond to geomagnetic energy sources