3D Modelling of the atmosphere of Pluto and...
Transcript of 3D Modelling of the atmosphere of Pluto and...
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3D Modelling of the
atmosphere of Pluto and
Triton
François Forget, Mélanie Vangvichith, Tanguy Bertrand, Jeremy Leconte
Laboratoire de Météorologie Dynamique (LMD), CNRS, Paris, France
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MercuryVenus
Earth
Mars
Titan
TritonAtmospheres in the solar system
•Terrestrial atmospheres Pluto
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PLUTO
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Pluto
• A surface covered by N2, CH4, CO ices + “Tholins”
• A strong seasonal cycle
– 1 year pluto = 247.7 Earth year
– Obliquity = 122°
– Perihelion = 29.6 AU/Aphelion=49.3 AU
• A thin Nitrogen atmosphere. Currently :
– Ps ~2 – 5 Pa (TBC)
– [CH4] ~0.5% (Lellouch et al. 2009)
(R~1200 km)
Thermal StructureStellar Ocultation (Elliot et al. 1989)
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New Horizons
478 kg
Decembre 2005
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New HorizonsFlyby
July 14, 2015
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New Horizon Payload (atm. Observations)
Haze & surface imaging Map surface ice & surface
temperatures + hazes
2 x solar occulation profiles(Temperature, aerosols)
Airglow
2 x atmospheric temperature profiles
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1) 3D Hydrodynamical core -> to compute large scale atmosphere motions and transport- Grid point model Typical resolution of 170 km- 25 vertical layers (10m, 20m, 40m,…160km)
2) Physical parametrizations-> to force the dynamic-> to compute the details of the local climate
T(z)Thermal molecularconduction
Flux from thermosphere(negligible on Pluto)
Convection
Possible Atm N2 + CH4 condensation
Surface N2 + CH4
condensation/sublimation
TurbulenceInternal heat flux
Subsurface conduction (18 layers)
With radiative transfer through CH4 and CO(with NLTE effects)
The LMD Pluto Global climate model
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• Thermal conduction in the high atmosphere :
– Semi-implicite scheme
– Flux assumed to negligible at the top
• Subsurface conduction
– Semi-implicite scheme
– 22 layers to account for Pluto timescales heat waves
• Turbulent mixing in the Boundary layer :
– Turbulent closure scheme based on Mellor and Yamada 2.5 parameterisation :
“Classical” parametrizations
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Condensation/sublimation of Nitrogen
• Surface condensation & sublimation - N2 condenses or sublime to conserve energy at N2 frost point…- special parameterization in sigma coordinates : (Forget et al, 1998)→ Condensation:
– the entire atmosphere is “pumped” into the ground. – “warm” air must be cooled
→ Sublimation : Cold and still air injected in the atmosphere
Bare Ground
Condensation Sublimation
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Gravitational tides from Charon
Navier-Stokes equation :
Vtide : gravitational potential caused by Charon's tides
a =distance Charon-Pluto,n = orbital angular velocitye = excentricity
l = latitude
f = longitude
Vwind < 1E-5 m/sdps=2E-2Pa-> Gravitational tides are assumed to be Negligible
tideVP
usionfDifolisiCorDt
vD
Vtide V07
8cos2 lcos(2f nt)
1
8cos2 lcos(2f nt)
3
4cos2 l
1
2
cosnt
ea
R
a
GMV PlutoCharon 3
2
0
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??Dilution by
subliming N2
Modelling the Methane cycle
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microphysics of N2-CH4 mixture neglected
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• Diurnal Thermal inertia set to 20 SI.
• Seasonal thermal inertia set to 500 USI
• Emissivity = 0.9 for all the three units
• Map with Buie et al, (1997) convention (Summer in the northern hemisphere in the 21st century).
We mostly assume the multi-terrain description of Pluto surface from Lellouch et al. 2000 (consistent with visible imaging, lightcurves, and visible and near-infrared spectroscopy).
CH4 ice : Alb = 0.408
Tholin/H2O mix Alb=0.100
N2 ice: Alb=0.657
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The key assumption: Initial map of
surface deposits
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V
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A challenge : long timescales
• Atm. Radiative timescale (10-20 years)
• seasonal heat storage in the subsurface
We start our simulation in 1980 with a “realistic” atmospheres, surface and subsurface temperatures, until 2015
Converged results after ~20 years (2008-2015) .
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Pluto’s Diurnal cycle in 2015
T(K)
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Thermal structure
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Mean Temperature profile: Comparison with observations and other models
Rad
ius (
km
)
Temperature (K)
1D model(Lellouch et al. 2009)
GCM
Zalucha et al. 2011
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Mean Meridional CirculationMass streamfunction (107 kg m-2 s-1)
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Mean Meridional Circulation IN THE LOWER ATMOSPHEREMass streamfunction (107 kg m-2 s-1)
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Mean Meridional CirculationMass streamfunction (107 kg m-2 s-1)
Thermal cell
Condensation flow
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m/s21
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Mean zonal wind in 2015
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Propagation of Thermal tides to the upper atmosphere(Signature detetected by stellar occulations (Toigo et al. 2010)
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Temperature anomaly at 0N 0E (K)
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Propagation of Thermal tides to the upper atmosphere(Signature detetected by stellar occulations (Toigo et al. 2010)
24Time (Pluto days)
Zonal zind anomaly at 0N 0E (m/s)
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Will New Horizons see Hazes and clouds ?
• Nitrogen Ice clouds? Probably not
• Methane ice clouds ?
• Photochemical organic Hazes ?
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??Dilution by
subliming N2
Modelling the Methane cycle
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microphysics of N2-CH4
mixture neglected
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CH4 Column averaged volume mixing ratio
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2015
Cloud condensation
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If one assume that CH4 ice clouds can nuclei on Pluto… (Assuming 100 Cloud condensation nuclei per kg of air)
Map of clouds (mostly in the low, cold atmosphere)
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2015 Methane ice column mean mixing ratio
Ice mixing ratiomol/mol %
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Ice mixing ratiomol/mol %
2010 Mean Methane ice column mean mixing ratio
~ Maximum Visible Optical depth
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Ice mixing ratiomol/mol %
CH4 ice Clouds could be detected at the limb near CO2 frost surfaces
This is sensitive to initial surface deposits
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Organic Hazes, like on Titan
See Rannou and Durry, 2009
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Cassini UV (false color)
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Titan-like aerosols formations
• Pathway to aerosols not very well known: [Lebonnois et al. (2002),
Wilson and Atreya (2003) and Lavvas et al (2008)]
• Hypothesis for Pluto: Aerosols generated by Lyman-αphotolysis of methane (CH3, CH2 , CH + N …) This provide an excellent estimation of Titan’s total aerosol
production (but not Triton?)
• Scheme for Pluto GCM1) Radiative transfer of Ly-α (Solar + Interplanetary: Gladstone et ql.
2015) precursor molecules in the upper atmosphere Transport2) Precursor convert to aerosols with characteristic decay time scale τ (a
fraction of C and N is added with C/N = 2). Transport & Sedimentation (monomers ~40 nm, ρ = 800 kg m-3)
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Direct conversion CH4+ hν aerosols
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Direct conversion CH4+ hν aerosols
ZOOM
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CH4+ hν precursors (τ=1.E7s) aerosols
Polar night
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CH4+ hν precursors (τ=1.E7s) aerosols
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CH4+ hν precursors (τ=1.E7s) aerosols
Cell strongly driven by N2 condensation
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However: the winter polar cap may not yet be condensing (Olkin et al. 2014, Young 2013)
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L. Young’s model
To explain the surface pressure increase detected by stellar occultations, it is necessary to account for a high seasonal thermal inertia, which prevent nitrogen to condense around the rotational south pole before 2050
• Observations— Model
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Haze on a Young & Olkin high thermal inertia Pluto
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• High seasonal thermal inertia (2000 SI below 3 cm, 20 SI above)• Low initial subsurface temperature (37K)• no condensation in the rotational south Pressure (strongly) increases ain the recent years expected
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Organic Haze on a Young & Olkin high thermal inertia Pluto
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??Dilution by
subliming N2
A fast volatile surface model derived from the Global Climate Model
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The atmospheric dynamics is replaced by an instantaneous mixing
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“Volatile Surface Model simulation” (Example)
MEDIUM thermal inertia:
I =400 SI
AN2 = 0.65ACH4 = 0.45ε = 0.9
Initially 50 kg m-2 of both ices everywhere
Time (Terrestrial years )
Time (Terrestrial years )
surface CH4 ice layer
surface N2 ice layer
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Evolution of modeled surface ices(CH4 ice , N2 ice)
~Observations in ~2000 using the same plotting system
“Volatile Surface Model simulation” (Example)
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Some results
with Triton’ GCM
Triton seen by Voyager 2, 1989
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TRITON ATMOSPHERE
• Atmosphere: N2 + 0.02 % CH4
• Surface pressure (1989) ~1.4 Pa, rising
• Some things we know about
Triton in 1989
– Surface dark streaks direction :
eastward surface wind in the
southern hemisphere
– Geyser like Plumes
• Westward wing ad ~8 km in the
southern hemisphere
• Tropopause around ~8 km
• What we don’t know well:
– Surface frost distribution (N2, CO,
CH4, …)
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New calculation of
Triton seasonal
variations required
to compute cap
evolution…
(Forget et al. 2000)
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Triton free atmosphere processes : hypothesis
• No radiative transfer below 40 km (Yelle et al.• Conduction : Temperature below 40 km insensitive to thermosphere variations (400 km)
Constant flux from thermosphere
400 km
60 km
40 km
Example of temperature profiles
Tmin Tmean Tmax
Diurnal cycle
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Triton General Circulation Model
1) Hydrodynamical code to compute large scale atmospheric motions
and transport
- Grid point model
- Horizontal resolution : ~200 km (32x24)
- 15 vertical layers (5m, 20m, … 50 km)
2) Physical parameterizations to force the dynamic
to compute the details of
the local climateT(z)
Thermal
conduction
Flux from
thermosphere
Convection
Surface N2 condensation
Atm N2 condensation
TurbulenceInternal heat
fluxSubsurface conduction (13 layers)
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• Bolometric albedo :
• Emissivity = 0.74• Thermal inertia =50 J m-2 s-1/2 K-1
• Flux géothermique nul• Ice Surface temperature = 38K• Initial temperature profile = isotherm
90°S 30°S 20°N 90°N
0.8
0.6
Mean temperature profiles for three different latitudes : 0°, 45°N and 45°S.
M. Vangvichith (LMD/ EDX)
Case 1 : Triton totally covered by N2 ice
Triton : atmosphere andsurface
Surface temperatureinversion
troposphere
thermosphere
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Case 1 : Triton totally covered by N2 ice
Angular momentum + Streamfunction (107 kg m-2 s-1)
Summer sublimation
Winter condensation
Retrograde winds
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Case 1 : Triton totally covered by N2 ice
Slide 27
Not consistent with Voyager 2 winds observations
No prograde winds (contrary to observations)
Retrograde surface winds
Plume( ~8km)
60°S
40°S
20°S
Wind streaks Surface→retrograde winds Plumes
(z~6-8km)→prograde winds
Observations
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• Ice bolometric albedo : 0.6 (dark ice)• Ground bolometric albedo = 0.8• Emissivity = 0.5• Thermal inertia =50 J m-2 s-1/2 K-1
• Flux géothermique nul• Ice Surface temperature = 38K• Initial temperature profile = isotherm
Not consistent with Voyager 2 winds observations
Case 2 : Frost free southern hemisphere
Frost free southern hemisphere (Spencer et al. 1990) (“Dark cap model”, Hansen and Paige 1992)
Case 2 : Frost free southern hemisphere
Triton : atmosphere and surface Atmosphere
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• Bolometric albedo :
• Emissivity = 0.74• Flux géothermique nul• Ice Surface temperature = 38K• Initial temperature profile = isotherm
• Initialisation of the band's temperature ?
90°S 30°S 20°N 90°N
0.8
0.6
Initialisation of the band's temperature :a serie of 1D simulations over more than 2000 terrestrial years for different values of thermal inertia
SURFA A
C TE
1T 5E °M NPERATURE
IT=50 uSI
IT=1000 uSI
IT (uSI) 50 200 500 1000
T in 1989 (K) 38 39.7 40 42
42 K
38 K
39.7 K
40 K
Case 3 : Triton with an unfrosted equatorial band
Triton : tmosphere and surface
Ingersoll et al. 1990
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M. Vangvichith (LMD/ EDX) May 31th, 2013 Slide 31Modeling of atmospheres/ices on Triton/Pluto
Case 3 : Triton with an unfrosted equatorial band
Triton : atmosphere and surface Atmosphere
Case with IT=1000 uSI
Temperature gradient between the equator and southern latitudes
Origin of prograde winds
Section of temperature in 1989
Mean zonal winds at 7 km (centered at 40°S)
Prograde winds
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• Thank you !