TUTORIAL Venus: The Atmosphere, Chemistry, and Clouds F.W. … · 2006-02-21 · Energy Balance of...
Transcript of TUTORIAL Venus: The Atmosphere, Chemistry, and Clouds F.W. … · 2006-02-21 · Energy Balance of...
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TUTORIAL
Venus: The Atmosphere, Chemistry, and Clouds
F.W. TaylorOxford University
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From ‘Physics and Chemistry of the Solar System’ by John S. Lewis
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• CO2 and N2 amounts ~‘same’ as the Earth• Water very low (⇒ loss rate is high)• D/H = 100 x Earth ⇒ possible ancient ocean• Abundant SO2, H2S, H2SO4 ⇒ active volcanism?• Some species are variable
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SO2 vs. Time (Na & Esposito, 1996)
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Model Venus temperature profile
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PioneerVenus OIRMeasured
Temperatures(3-month
mean)vs.
Height & Longitude
at 0o latitude
(Schofield & Taylor, 1982)
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PioneerVenus OIR
Temperatures vs.
Height & Longitude
Solar Tide
- wavenumber 2 in stratosphere
- wavenumber 1 at cloudtops
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Pioneer Venus OIR Temperatures vs. Height and Latitude
55km
105km
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Pioneer Venus OIR Temperatures vs. Height and Latitude
Temperature increases from equator to pole!
Polar collar
Polar Dipole
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POLAR COLLAR POLAR DIPOLE
IR (12.5 µm)UV
Fourviews
ofthe
NorthPolarregion
ofVenus
(M10 TV,PV OIR)
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The variation with latitude of carbon monoxide abundance near 30 km altitude (Collard et al., 1994).
COmixingratio,ppmv
Galileo NIMS data
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Conceptual model for CO sources on Venus: transport from the upper atmosphere via the polar vortices.
Hei
ght
Latitude
N Pole Equator S Pole
Very High CO
Low CO
High CO
Volcano
clouds
Transport in polar vortex
CO Sink at surface
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Profile of the clouds from the PV large probe(RG Knollenberg and DM Hunten,1980)
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From ‘Physics and Chemistry of the Solar System’ by John S. Lewis
Atmospheric Chemistry dominated by Sulfur?
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The ‘Ashen Light’ of Venusfirst observed by Giovanni Riccioli on January 9, 1643
[P. Moore]
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… at 2.3 microns
D. Crisp, NASA/JPL
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Venus Near-IR Spectrum
Observations (Allen and Crawford, 1984)
240 Kblackbody
Model (Kamp, Taylor & Calcutt, 1988)
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Galileo NIMS view of
mysterious ‘weather’ in the deep atmosphere
of Venus(Carlson et al.)
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Energy Balance of the EarthApplying the Stefan-Boltzmann law we obtain for the total radiant power of the Sun, with temperature TS & radius RS:
ESun = 4πRS2 σ(TS)4 = 4π S RES
2
where S is the solar constant and RES the distance Earth –Sun. Now:EE = 4πσ RE
2 (TE)4 = (1-A) S π RE2
→ radiometric temperature of the Earth TE = 255 K.
The mean surface temperature of the Earth is about 288 K.The difference is due to the fact that only a small part of the thermal emission to space takes place from the surface; most is from the colder regions near the tropopause.
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Energy Balance of VenusApplying the Stefan-Boltzmann law we obtain for the total radiant power of the Sun, with temperature TS & radius RS:
ESun = 4πRS2 σ(TS)4 = 4π S RVS
2
where S is the solar constant and RES the distance Earth –Sun. Now:EV = 4πσ RV
2 (TV)4 = (1-A) S π RV2
→ radiometric temperature of Venus TV = 240 K.
The mean surface temperature of Venus is about 760 K.The difference is due to the fact that only a small part of the thermal emission to space takes place from the surface; most is from the colder regions near the tropopause.
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Jenkins, 1995
Magellan radio occultation temperature profile
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Jenkins, 1995
Radiative-convective equilibrium model
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Why is Venus so hot?
- CO2 is in equilibrium with carbonates on surface (Urey, 1952)
- the dominant reaction is expected (Bullock & Grinspoon 1996) to be
CaCO3 + SiO2 ⇔ CaSiO3 + CO2
- use thermodynamic data (e.g. Adamik and Draper, 1963) for the temperature dependence of the pressure of CO2 in the form
log P = ΔH/RT +ΔS/R + A + BT + CT-2
- use the radiative-convective equilibrium model for the surface pressure as a function of surface temperature
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Summary Part 1:
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Summary Part 2:
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More data! More data! From pole to equator!Measure everything, everywhere, all of the time!