¾At hä D ik Atmosphären: Dynamik - dlr.de · Sources of dynamical variability in the Earth‘s...
Transcript of ¾At hä D ik Atmosphären: Dynamik - dlr.de · Sources of dynamical variability in the Earth‘s...
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Ringvorlesung „Planeten und Leben im Überblick“, TU Berlin, 28. Mai 2009
ÜRingvorlesung „Planeten und Leben im Überblick“
Oberflächen …..
At hä D ikWasser …..Atmosphären: DynamikAtmosphären: ChemieAtmosphären: Chemie
Atmosphären: Klimaentwicklungp gInneres …..
Institut für Meteorologie, Freie Universität Berlin
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Ringvorlesung „Planeten und Leben im Überblick“, TU Berlin, 28. Mai 2009
Atmosphären: Dynamik
Dynamik und TransportprozesseDynamik und Transportprozesse in Planetenatmosphären
Prof Dr Ulrike LangematzProf. Dr. Ulrike LangematzInstitut für Meteorologie, Freie Universität Berlin
Dr. Lee GrenfellZentrum für Astronomie und Astrophysik, Technische Universität Berlin
Institut für Meteorologie, Freie Universität Berlin
Zentrum für Astronomie und Astrophysik, Technische Universität Berlin
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D i l tDynamical aspects f ‘of the Earth‘s
atmosphere
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Bild kann nicht angezeigt werden. Dieser Computer verfügt möglicherweise über zu wenig Arbeitsspeicher, um das Bild zu öffnen, oder das Bild ist beschädigt. Starten Sie den Computer neu, und öffnen Sie dann erneut die Datei. Wenn weiterhin das rote x angezeigt wird, müssen Sie das Bild möglicherweise löschen und dann erneut einfügen.1 The sun as energy source
Dynamical aspects of the Earth‘s atmosphere
Differential solar heating1. The sun as energy source Differential solar heatingTemperature gradients
Dynamics
Factors affecting dynamics:• Orbital parameters
11-year Schwabe-Zyklus• Orbital parameters • Rotation of planet • Variability of energy input
0 1 %0.1 %Maunder Minimum
http://www.pmodwrc.ch/solar_const/solar_const.html1645-1715 Hoyt und Schatten, 1993, updated
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2 Chemical composition of Earth‘s atmosphere
Dynamical aspects of the Earth‘s atmosphere
Substance Fraction [V%]
2. Chemical composition of Earth s atmosphere
Nitrogen (N2) 78,08
Oxygen (O2) 20,95
Argon (Ar) 0,93g ( ) ,
Carbondioxid (CO2) 0,033
Neon (Ne) (+ Noble gases) 90%
10%dry
Factors affecting dynamics:moist• chemical compositionJanuary, ppmv
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Dynamical aspects of the Earth‘s atmosphere
Short wave solar heating ratedue to absorption by ozone and
Temperaturein °Cdue to absorption by ozone and
molecular oxygenin K/day
in C
January
KW
W
KK
K
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Dynamical aspects of the Earth‘s atmosphere
1. Radiative equilibrium in the stratosphere in summer.
Zonal gemittelte Temperatur
2. zonally symmetric irradiance
→ 2-d approximation valid
1. Dynamical disturbances in the winter stratosphere and in the mesosphere
2. longitudinal dependence
→ 3-d dynamics
Theoretical concept of zonal mean background state with imposed
summer winter
Theoretical concept of zonal mean background state with imposed dynamical effects by wavelike disturbances
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Temperature and zonal windDynamical aspects of the Earth‘s atmosphere
E
Temperature and zonal wind
January, zonal means
How does the corresponding zonal wind field look like?
W ESPARC climatology(http://sparc.sunysb.edu)
Polar night jet
With the assumption of geostrophic balance: WE
Polar night jet
Equilibrium between Coriolis force (due to Earth rotation) and pressure gradient force in the large scale):
W
Egradient force in the large scale):
Geostrophic wind:
u = −1/(ρf) δp/ δyu 1/(ρf) δp/ δy
Thermal wind:
δ /δ δT/δ
W W
δu/δz = ~ − δT/δy
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Stratospheric mean circulationDynamical aspects of the Earth‘s atmosphere
winter
Geopotential height, long-term mean, northern hemisphere
Stratospheric mean circulation
summerwinter summer
H
T H
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Episodic occurrences of Major Stratospheric Warmings
Dynamical aspects of the Earth‘s atmosphere
Episodic occurrences of Major Stratospheric Warmings
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Ringvorlesung „Planeten und Leben im Überblick“, TU Berlin, 28. Mai 2009
Arctic high in summer Stratospheric warming im Januar 2006
2d-approximation valid 3d-dynamics)tz(u)tz(u ϕ≈ϕλ )tz('u)tz(u)tz(u ϕλ+ϕ=ϕλ
Institut für Meteorologie, Freie Universität Berlin
)t,z,(u)t,z,,(u ϕ≈ϕλ )t,z,,(u)t,z,(u)t,z,,(u ϕλ+ϕ=ϕλ
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Zwischenjährliche Variabilität in der StratosphäreDynamical variability of the stratosphere in winterDynamical aspects of the Earth‘s atmosphere
j py y pSeasonal evolution of stratospheric North Pole temperature
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Sources of dynamical variability in the Earth‘s atmosphere I
Dynamical aspects of the Earth‘s atmosphere
Sou ces o dy a ca a ab y e a s a osp e e
Excitation of large-scalePlanetary wavesPlanetary wavesRossby wavesKelvin wavesKelvin waves
at the surface byh• orography
• land-sea contrast
or in-situ atmospheric instability
stationary or transient
dependent on ωdependent on ωLaboratory experiments in a water tank with different rotational speed(Hide and Mason, 1975)
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Sources of dynamical variability in the Earth‘s atmosphere II
Dynamical aspects of the Earth‘s atmosphere
Sources of dynamical variability in the Earth s atmosphere II
Excitation of
Gravity wavesGravity waves
at the surface by• orography• orography
in the atmosphere byconvection• convection
• shear winds
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Equator-to-Pole Transport Cells
PolarE th FerrelEarth
H dlHadley(not to scale)
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Dynamical aspects of the Earth‘s atmosphere
Shaded:Area with strong wave dissipation: Surf zone
Breaking planetary and gravity waves in
Wave driven pump Surf zoneand gravity waves in
the upper stratosphere drive the
pump
mean meridional circulation.
in the stratosphere in winter
Holton und Alexander (2000)
Equator Winter Pole
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M idi l i l ti (MMC)
Dynamical aspects of the Earth‘s atmosphere
Mean meridional circulation (MMC)Brewer-Dobson-Zirkulation (BDC)
70km
10km10km
summer winter
The BDC describes the net meridional mass transport in the atmosphere.
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Transport characteristics from long-lived trace gasesDynamical aspects of the Earth‘s atmosphere
p g g
HALOE t llit d tHALOE satellite data
2
1
1. Tropical upwelling
2. Downwelling at high latitudes
3
latitudes
3. Flat gradients in surf-zone due to redistribution by waves
4. : Polar, subtropical transport barriers
Randel (2001)HF: Wasserstoff-Fluorid
Quelle: Stratosphäre
transport barriers
Randel (2001)Quelle: Stratosphäre
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Another example: Ozone
Dynamical aspects of the Earth‘s atmosphere
Another example: OzoneSBUV: Jahresmittel von 1980-89, Ozon (DU/km)
Ozone is transported from photochemical source regions in the upper tropical stratosphere to high latitudes in the lower stratosphere by the BDC.
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Zunahme der Gesamtozonsäule in hohen Breiten im WinterDynamical aspects of the Earth‘s atmosphere
infolge Transport mit der Brewer-Dobson-Zirkulation(Dobson et al., Proc. Roy. Soc. London, 1929)
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Specific transport
Dynamical aspects of the Earth‘s atmosphere
Specific transport phenomena: The tropical QBOThe tropical QBO
QBO: Quasi-biennial Oscillation
of the tropical zonal wind in the middle stratosphere
F d f th l t hForced from the lower atmosphere by vertically propagating waves
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Transport of trace gases with the atmospheric circulationp g p
WMO (1999)WMO (1999)
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Ringvorlesung „Planeten und Leben im Überblick“, TU Berlin, 28. Mai 2009
Dynamical regimes y a ca eg esof other planetsof other planets
Institut für Meteorologie, Freie Universität Berlin
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Ringvorlesung „Planeten und Leben im Überblick“, TU Berlin, 28. Mai 2009
Mars Venus andMars, Venus and othersothers
Institut für Meteorologie, Freie Universität Berlin
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Ringvorlesung „Planeten und Leben im Überblick“, TU Berlin, 28. Mai 2009
VENUS – EARTH - MARS
Planetary Data
Radius(km) 6052 6360 3395Mass (kg) 4.87x1024 5.97x1024 6.42x1023
Gravity (m/s2) 8 87 9 81 3 71Gravity (m/s2) 8.87 9.81 3.71Distance from Sun (AU) 0.72 1.0 1.52Obliquity (degrees) 177.4 23 25.2L th Y (E th d ) 224 7 365 25 687 0Length Year (Earth days) 224.7 365.25 687.0Length Day (Earth days) -243.0 1.0 1.03Number of Satellites 0 1 2Eccentricity 0.0067 0.0167 0.093Inclination (degrees) 3.4 0.0 1.9Visual Albedo 0.65 0.4 0.15
Institut für Meteorologie, Freie Universität Berlin
Surface T (K) 735 288 220Surface P (bars) 93 1.0 0.006
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Ringvorlesung „Planeten und Leben im Überblick“, TU Berlin, 28. Mai 2009
Institut für Meteorologie, Freie Universität Berlin
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Ringvorlesung „Planeten und Leben im Überblick“, TU Berlin, 28. Mai 2009
Mars Orbit and ClimateMars Orbit and Climate
Mars is ~half the size of Earth and only ~11% of the mass! Weaker gravity has resulted in stronger escape
1.38AU 1.65AU
resulted in stronger escape hence a thin atmosphere.
Mars’ orbit is more eccentric45% change
Mars orbit is more eccentric compared with the Earth so strong climate effects are
in solar input
gexpected.
Institut für Meteorologie, Freie Universität Berlin
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Ringvorlesung „Planeten und Leben im Überblick“, TU Berlin, 28. Mai 2009
Mars Orbit and Climatea s O b a d C a e
Mars Orbit not only eccentric but also large
Institut für Meteorologie, Freie Universität Berlin
variations in obliquity – strong climate changes
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Ringvorlesung „Planeten und Leben im Überblick“, TU Berlin, 28. Mai 2009
Martian Surface – Mercator Viewa a Su ace e ca o e
Vastitas Borealis (~-4km)OlympusAlbaPhoenix ( )Olympus
MonsPatera
Viking 2
ElysiumViking 1
SyrtisPathfinder
Tharsis (~+4km)Hellas
SpiritMajor
Opportunity
Argyre
HellasBasin
gy
Institut für Meteorologie, Freie Universität Berlin
Mars Orbiter Surface Altimeter (MOLA)
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Ringvorlesung „Planeten und Leben im Überblick“, TU Berlin, 28. Mai 2009
Mars’ Atmosphere
Institut für Meteorologie, Freie Universität Berlin
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Ringvorlesung „Planeten und Leben im Überblick“, TU Berlin, 28. Mai 2009
Mars: Atmospheric T P ProfileMars: Atmospheric T-P Profile
Atmosphere is thin (6mb) and cold (~250K) at surface
Water frozen out of atmosphereatmosphere
Dusty Climate
Mainly CO2 (95.3%)
Seasonal Pressure Cycle
Institut für Meteorologie, Freie Universität Berlin
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Ringvorlesung „Planeten und Leben im Überblick“, TU Berlin, 28. Mai 2009
Martian Seasonal Pressure Cycley
CO2 condenses in polar regions in winter leads to
Institut für Meteorologie, Freie Universität Berlin
20% variation in atmospheric pressure (cf 1% on Earth)
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M ti At h i D iMartian Atmospheric Dynamics
Important Principles
No ocean (strong heat sink on Earth)strong cyclical variations
e g temperature driven by changes ine.g. temperature driven by changes insolar insolation and
Obliquity and eccentricity are strongly variable affect Martian climate
Institut für Meteorologie, Freie Universität Berlin
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Ringvorlesung „Planeten und Leben im Überblick“, TU Berlin, 28. Mai 2009
Martian Daily Temperature CycleMartian Daily Temperature Cycle
Driven by solar input and radiative properties of surface.
Institut für Meteorologie, Freie Universität Berlin
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Ringvorlesung „Planeten und Leben im Überblick“, TU Berlin, 28. Mai 2009
Seasonal Temperature Changes on Mars
VIKING 1 (~20N)
VIKING 2 (~50N)
Institut für Meteorologie, Freie Universität Berlin
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Seasonal Temperature Changes on MarsLarge Dust Storm causes weakening of T amplitude
Seasonal Temperature Changes on Mars
VIKING 1 (~20N)
VIKING 2 (~50N)
Institut für Meteorologie, Freie Universität Berlin
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Ringvorlesung „Planeten und Leben im Überblick“, TU Berlin, 28. Mai 2009
Hadley Cell on MarsHadley Cell on Mars
• smaller Coriolis force• smaller Coriolis force• single, giant Hadley cellcan form
• Faster on MarsMars – 100 daysEarth – 1 year
Cell is “slowed” byheat absorption fromheat absorption fromoceans on Earth
Institut für Meteorologie, Freie Universität Berlin
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Mars• smaller Coriolis force• single giant Hadley cell
Mars• single, giant Hadley cellcan form
• Faster on MarsMars – 100 daysEarth – 1 year
Cell is “slowed” byheat absorption fromheat absorption fromoceans on Earth
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Ringvorlesung „Planeten und Leben im Überblick“, TU Berlin, 28. Mai 2009Modelling the Martian Hadley Cell
Modern Mars
Vary Orbit Parameters
R O hRemove OrographyBIGGEST EFFECT!
Institut für Meteorologie, Freie Universität Berlin Richardson and Wilson (2002)
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3D (GCM) Zonal mean Temperature of Mars3D (GCM) Zonal mean Temperature of Mars
W i iWarm region arisesdue to atmospheric waves formed near the surfaceformed near the surfacetravelling polewards,breaking and depositing heat
Winter Summer
Source: Mars Atmosphere Observation and Modelling
Institut für Meteorologie, Freie Universität Berlin
Source: Mars Atmosphere Observation and Modelling
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Ringvorlesung „Planeten und Leben im Überblick“, TU Berlin, 28. Mai 2009
GCM Si l ti f M l i dGCM Simulation of Mars zonal wind
strong wintertimepolar vortex developspolar vortex developsdue to meridional flow
WinterSummer
Institut für Meteorologie, Freie Universität Berlin
WinterSummer
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Ringvorlesung „Planeten und Leben im Überblick“, TU Berlin, 28. Mai 2009
Atmospheric Dynamics on VenusAtmospheric Dynamics on
Cyclostrophic flow – Coriolis force weak -
VenusCyclostrophic flow Coriolis force weak Pressure force balanced by centrifugal force
CentrifugalForce
Coriolis and small CentrifugalF
Wind
PressureGradient Force
Wind
Force PressureGradient Force
d
V E thVenusZonal Cyclostrophic Wind
EarthZonal Geostrophic Wind
Institut für Meteorologie, Freie Universität Berlin
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Ringvorlesung „Planeten und Leben im Überblick“, TU Berlin, 28. Mai 2009
Meridional Transport on Earth and VenusMeridional Transport on Earth and Venus
LESS HEAT ABSORBED BY VENUSLESS HEAT ABSORBED BY VENUSBECAUSE ALBEDO=0.6 (Earth=0.4)
Institut für Meteorologie, Freie Universität Berlin
Weak meridional heat gradient on VenusSource: LASP
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Ringvorlesung „Planeten und Leben im Überblick“, TU Berlin, 28. Mai 2009
Venus N-S transport from single giant Hadley Cell
Earth – fast rotationt C i li fstrong Coriolis force
“breaks” circulationinto three cells(Hadley, Ferrel, Polar)
Venus slow rotationVenus – slow rotation,thick atmosphere – singleHadley cell is stabley
Institut für Meteorologie, Freie Universität Berlin
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Ringvorlesung „Planeten und Leben im Überblick“, TU Berlin, 28. Mai 2009
Venus N-S transport from single giant Hadley Cell
Earth – fast rotationt C i li fstrong Coriolis force
“breaks” circulationinto three cells(Hadley, Ferrel, Polar)
Venus slow rotationVenus – slow rotation,thick atmosphere – singleHadley cell is stable
Venus Express Missionhas updated knowledge in this region y-the Hadley cell extends only up to-60o THEN there is a double (dipole) vortex
Institut für Meteorologie, Freie Universität Berlin
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Venus e us
• Vertically overlappingcellscells
• Twin polar vortices• Superrotation ofatmosphere
Source: Ruslike 2007
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Ringvorlesung „Planeten und Leben im Überblick“, TU Berlin, 28. Mai 2009
Venus has “superrotation”Venus has superrotation
wind slower near poles
St i d
E W Winds ~100ms-1 at
Strong windsat cloud topsin tropicsE W Winds 100ms-1 at
~60km 60 timesfaster than planet in tropics
Weak surfacewinds
p
tropicsi.e. SUPERROTATION
winds
Institut für Meteorologie, Freie Universität Berlin
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Ringvorlesung „Planeten und Leben im Überblick“, TU Berlin, 28. Mai 2009
St di f V ’ S t tiStudies of Venus’ Superrotation
Problem – to simulate superrotation needs a mechanismto transfer angular momentum from surface to atmosphere.Difficult for models!!! Some examples of model studies:
• Hourdin et al (1992) – produced superrotation inHourdin et al. (1992) produced superrotation innon-forced LMD (French) GCM
•Del Genio et al. (1993) – superrotation from upper tropospherecloud radiative effect in GCM
Institut für Meteorologie, Freie Universität Berlin
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Ringvorlesung „Planeten und Leben im Überblick“, TU Berlin, 28. Mai 2009
Titan
Institut für Meteorologie, Freie Universität Berlin
Source: Cassini Source:Huygens
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Ringvorlesung „Planeten und Leben im Überblick“, TU Berlin, 28. Mai 2009
Why study Titan’s atmosphere?
Only body in solar system other than Earth withOnly body in solar system other than Earth with thick (1.5 bar) nitrogen atmosphere
Conditions are thought to resemble the early Earth so understanding Titan could shed light on earthlike atmosphere development andearthlike atmosphere development and conditions favouring life
Institut für Meteorologie, Freie Universität Berlin
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Ringvorlesung „Planeten und Leben im Überblick“, TU Berlin, 28. Mai 2009
Titan's atmosphereTitan s atmosphere
Surface T=94KSurface T 94KSurface P=1.5bar97% N23% CH4
Resembles EarlyResembles Early Earth
Institut für Meteorologie, Freie Universität Berlin
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Ringvorlesung „Planeten und Leben im Überblick“, TU Berlin, 28. Mai 2009
Titan GCM Studies
(Superrotation in upper atmosphere)( p pp p )
Source: Samuelson (2002)
Institut für Meteorologie, Freie Universität Berlin
Source: Samuelson (2002)
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Ringvorlesung „Planeten und Leben im Überblick“, TU Berlin, 28. Mai 2009
Summary of atmospheric dynamical regimesy p y g
Institut für Meteorologie, Freie Universität Berlin
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Ringvorlesung „Planeten und Leben im Überblick“, TU Berlin, 28. Mai 2009
Saturn’s Hexagonal Vortex at high Northern latitudes…g g
S CSource: Cassini
Feature is long-lived
Institut für Meteorologie, Freie Universität Berlin
observed by Voyager and recently by Cassini
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Jupiter’s global atmospheric dynamicsTemperature (K)Temperature (K)
Values oscillate with4 i d (Q i4-5 year period (QuasiQuadrennial Oscillation (QQO)
equator colder thanmid-lats!
(QQO)
Zonal Wind (u,ms-1)
mid-lats!
( )from thermal windrelation (i.e. u
proportional to dT/dlat)
Source:Fl t l (2004)
proportional to dT/dlat)strong jet
Flasar et al. (2004)Cassini data
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Ringvorlesung „Planeten und Leben im Überblick“, TU Berlin, 28. Mai 2009
Jupiter’s hotspot at 1mbat 1mb
1mbHOTSPOT Purple = 160K
Red = 185KRed = 185K
SSource:Flasar et al. (2004)
Cassini data4mb
NO HOTSPOT
Institut für Meteorologie, Freie Universität Berlin
O O S O
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Atmospheric Transport on the Early Earthy
What do we know:
• Thick atmosphere (~1-10 bar)• High CO2 (~x100 present from sediment data)• ~30% weaker sun (stellar models) (but UV probably higher)
CO H H O CH f i d l t di• CO, H2, H2O, CH4 from previous model studies• Earth spun about 50% faster
Moon was up to 15 times closer• Moon was up to 15 times closer
ATMOSPHERE PROBABLY V DYNAMICALLY PERTURBED!!ATMOSPHERE PROBABLY V. DYNAMICALLY PERTURBED!!