Planetary atmosphere modellingand other activities at LMD, IPSL	François Forget and the LMD« Planetogy » team
CNRS, Institut Pierre Simon Laplace, Laboratoirede Météorologie Dynamique, Paris

Planetary Science in « Laboratoire de MétéorologieDynamique » (LMD) within Institut Pierre Simon Laplace (IPSL)In the Paris aera, France	  •	  LMD	  =	  «	  Laboratory	  for	  Dynamic	  Meteorology	  :	  A	  department	  (~200	  persons)	  	  	  _	  Atmospheric	  Sciences:	  theories,	  modeling	  	  and	  observa7ons	  •IPSL	  =	  «	  Ins7tut	  Pierre	  Simon	  Laplace	  »	  	  	  	  	  	  	  	  	  	  	  	  =	  A	  federa7on	  of	  	  7	  «	  laboratories	  including	  »	  	  LMD	  	  	  (~1200	  persons)	  in	  the	  Paris	  aera	  _	  Environmental	  	  Sciences:	  ocean,	  biosphere,	  atmosphere,	  	  chemistry,	  	  paleoclimates,	  planetary	  sciences	  •	  CNRS	  =	  The	  big	  Na7onal	  administra7on	  which	  coordinate	  french	  research	  and	  pays	  civil-­‐servant	  scien7st	  salaries	  (unless	  they	  are	  professor	  in	  Universi7es)	  •	  UPMC	  =	  University	  Pierre	  &	  Marie	  Curie:	  The	  Big	  University	  where	  our	  oﬃces	  are	  and	  which	  pays	  Professors	  	  like	  Aymeric	  Spiga.	  
2	

Numerical modelling of Earthclimate at LMD and IPSLPlanetary Sciences at IPSLThe « Solar SystemCenter »•~80 permanent scientists and engineers et ~60
contractors (post-doc, students, engineers) working on
Planetary Sciences•3 main topics :1. Climate and Meteorology on other planets
2. Interaction Sun – Planets - Earth
3. Origins of Planets and Life.

Topic	  #1	  :	  	  Climate	  &	  météorology	  on	  terrestrial	  planets	  	  Space-­‐based	  	  observa7ons	  &	  Climate	  Modelling	  	  • Mars	  Mars	  Vénus	  – Space	  Mission	  :	  Mars	  Express	  (instrument	  SPICAM,	  «	  IDS	  »,	  Co-­‐Is)	  :	  LATMOS	  +	  LMD	  a	  ESA	  Exomars,	  Insight	  (2016,	  2018)	  – Modelling	  :	  	  «	  Mars	  system	  simulator	  »,	  méso/micro-­‐scale:	  LATMOS	  +	  LMD	   	  	  • Venus	  – Space	  Mission	  :	  Venus	  Express	  (instrument	  SPICAV-­‐SOIR	  (LATMOS),	  Co-­‐Is)	  :	  LATMOS	  +	  LMD	  – Modelling	  :	  GCM	  Venus:	  LATMOS	  +	  LMD	  Titan	  • Titan	  – Space	  Mission:	  Cassini	  Huygens	  (PI,	  coIs)	  – Modelling	  :	  “IPSL”	  Titan	  GCM	  	  	  (LMD	  +	  GSMA)	  • Exoplanets	  &	  past	  atmospheres	  – Modelling:	  «	  Generic	  »	  GCM	  (LMD,	  LATMOS)	  a	  Space	  telescope	  Echo	  (ESA,	  preselected)	  Topic #2 :Interac7on Sun – Planets – Earth• Interac7on	  	  solar	  wind	  	  -­‐	  exosphere	  -­‐	  	  atmospheres	  	  	  _	  Atmospheric	  Escape	  • Heliosphere	  and	  solar	  wind	  studies	  Numerical Simulations

Space Obs.: UV and Mass spectrometers

Ex:	  -­‐	  SOHO/SWAN	  (Sun)	  Modelling	  exospheres	  &	  interac7ons	  with	  solar	  wind	  •	  Earth	  •	  Mars	  	  	  	  	  	  	  	  	  	  	  	  	  	  	  	  	  (_	  Mars	  Express;	  Maven)	  •	  Mercury	  	  	  	  	  	  	  	  	  	  	  (_	  Bepi	  Colombo)	  •	  Ganymede	  	  	  	  	  	  	  (_	  JUICE)	  -­‐	  Cassini:	  around	  Saturn	  (and	  Titan)	  since	  2004	  	  	  -­‐	  RoseRa	  (launch:	  2004:	  Comet	  in	  2014).	  See	  below.	  

-­‐Bepi-­‐Colombo	  :	  Mercury	  (launch	  	  2015)	  (LATMOS)	  	  	  PI	  	  UV	  spectrometer	  PHEBUS	  	  (UV	  spectro	  	  &	  co-­‐PI	  PICAM	  	  -­‐	  MAVEN	  	  (Mars,	  	  launched	  2013)	  :	  see	  below	  -­‐	  TARANIS	  	  (Earth):	  see	  below	  	  (2015)	  -­‐	  JUICE	  (Jupiter	  2022):	  Mass	  Spectro	  NIMEIS	  ,	  LATMOS	  	  (F.	  
Leblanc)	  on	  instrument	  su7e	  JUMMP	  (Pi:	  Coates)	  Topic #3 :Origins of Planets and Life.
• To understand solid body formation by studying comets, asteroids andinterplanetary dust.
• To study extraterrestrial organic matters and its evolution. (e.g. Mars, Titan).

Space experiments (mostly in-situ)

Laboratory simulations

SAM Gas Chromatograph on Curiosity•	  In-­‐situ	  	  Analysis	  (LATMOS-­‐LISA)	  -­‐Gas	  Chromatograph:	  SAM	  (Curiosity),	  GAP	  (Phobos-­‐Grünt	  2011)	  ,	  COSAC	  	  (Roseha,	  Comet)	  MOMA	  (Exomars	  Rover	  2018)	  +	  COSIMA	  (dust	  analyser,	  Roseha)	  -­‐Radar	  	  (LATMOS):	  	  	  •	  Consert	  +	  Permi7vity	  probe	  (Roseha)	  •	  Wisdom	  (Exomars	  Rover2018)	  •	  	  Simula7ng	  photochemistry	  on	  Titan	  and	  organic	  aerosols.	  	  	  	  Experiments	  PAMPRE	  (LATMOS),	  PLASMA,	  SETUP	  (LISA),	  SMARD	  (LATMOS,+LISA)	  	  	  •	  Physic	  of	  space	  ices	  :	  experiments	  OREGOC	  (LISA),	  SPICES	  (LPMAA)	  •	  	  Physico-­‐chemistry	  of	  Mars	  surface	  ExperimentsMOMIE	  (LISA+	  LATMOS)	  Modelling	  of	  Planetary	  	  Climates	  at	  LMD	  and	  IPSL	  A hierarchy of models for planetary climatology
1. 1D global radiative convective models[ Great to explore a wide range ofpossible climates; (e.g. Kasting et al. 1993 )2. 2D Energy balance models…
3. Theoretical 3D General Circulation
model with simplified forcing: used toexplore and analyse the possible
atmospheric circulation regime(seeRead 2011, Heng et al. 2011Showman et al. 2013, etc)

4. Full Global Climate Models aiming atbuilding “virtual” planets.

Ambitious Global Climate models : Building “virtual”
planets behaving like the real ones, on the basis ofuniversal equations
Observations

RealityModels

How to build a full Global
Climate Simulator ?
Earth System Model (CESM),:How to build a full Global
Climate Model :1) Dynamical Core tocompute large scaleatmospheric motionsand transport2)	  Radia7ve	  transfer	  through	  gas	  and	  aerosols	  3)	  Turbulence	  and	  convec7on	  in	  the	  boundary	  layer	  4)	  Surface	  and	  subsurface	  thermal	  balance	  	  6)	  Photochemical	  hazes	  &	  mineral	  dust	  5)	  Vola7le	  condensa7on	  on	  the	  surface	  and	  in	  the	  atmosphere	  	  Forget and Lebonnois (2013) In“ComparativeClimatology of Terrestrial

How to build a Global
Climate Model :Atmospheres in the solar system

TritonPluto•Terrestrial atmospheres
TitanMars
EarthMercury

Venus

GCMs at LMD/IPSL

MARS
VENUS

EARTH
Applications:• Climatology• Climate projections• Paleoclimates• chemistry• Biosphere /hydrospherecryosphere / oceans
coupling• Many otherapplications

TRITON

PLUTO

Coupled cycles:• CO2 cycle• dust cycle• water cycle• Photochemistry• thermosphere andionosphere• isotopes cycles•etc…
Applications:Dynamics,
assimilation;
paleoclimates, etc…
•TITANThe LMD/IPSL « Mars system simulator »AtmosphericDynamicsExosphereAtm. Escape(Latmos, LMD)

CO2 Cycle(LMD, Latmos
IDES)

MarsGCM
Dust cycle(Oxford U., LMD,
LISA, Latmos)

Thermosphere
Ionosphere(Latmos, IAA)

« Mars Climate database »• Reference tool for the
Scientific and Space Engineercommunity• Version « pro » on DVDROM ordered par ~250 teams
from ~20 countries• Interactive website

Climate variations& paleoclimates(LMD, Brown U, IDES.)

Volcanic eruption
simulations(with Brown University)(IAA, LMD,Latmos)-Mesoscale
Model / LES(LMD)

PhotoChemistry

Water Cycle
Radon Cycle

HDO cycle(Latmos, Lesia)(LMD, Latmos)

Ancient Mars(- 3 à -4 Gyr(avec Harvard University
Obs. Royal de Belgique)(IAA=Institut d’Astrophysique d’Andalousie)

GCMs at LMD/IPSL

MARS
VENUS
Coupling dynamic &radiative transfer +cloud physics +photochemistry	TRITON

PLUTO

GCM

GCM

EARTH
Applications:• Climatology• Climate projections• Paleoclimates• chemistry• Biosphere /hydrospherecryosphere / oceans
coupling• Many otherapplications

Coupled cycles:• CO2 cycle• dust cycle• water cycle• Photochemistry• thermosphere andionosphere• isotopes cycles•etc…
Applications:Dynamics,
assimilation;
paleoclimates, etc…
•TITAN
Coupling dynamic &radiative transfer +Coupled cycles:• Aerosols• Photochemistry• Clouds• Paleoclimates	

Atmospheres in the solar system

NEPTUNE• GIANT PLANETSURANUS
SATURNEJUPITERJupiterSaturn’s stratosphere Thermal wind field

Data Cassini CIRS, Fouchet et al. 2008

Cassini
Saturne : A well observed
atmosphère.
Combined with modern
computing : Toward a Giantplanet GCM.

Project « Emergiants » at LMD
Challenge: - Resolutions- Long runs
- Boundary conditions

A. Spiga
S. Guerlet
M. Indurain
M. Sylvestre	Atmospheres in the solar system

TritonNEPTUNE

Pluto• GIANT PLANETS• Terrestrial atmospheres

URANUS

Titan
JUPITERMars
EarthMercuryVenus

SATURNEAtmospheres in the solar system

TritonPluto• GIANT PLANETS• Terrestrial atmospheres
Titan

Mars
Earth
Mercury

Venus

Atmospheres in the solar system

TritonPluto• GIANT PLANETS• Terrestrial atmospheres
Titan

Mars
Exoplanets

EarthMercuryVenus

Why are we here today ?
• To collaborate and exchange ideas onmodelling & planetary exploration…
In particular:_ Brainstorm with you on the future ofplanetary climate modelling

The future of planetary climate
modelling: Some ideas• Improved dynamical cores & high parallelism_Toward very high resolution for global models

The future of planetary climate
modelling: Some ideas• Improved dynamical cores & high parallelism_Toward very high resolution for global models• Improved « parameterization » of climate
processes– More universal physics, less assumptions…
– Design of Parameterizations + careful independanttuning using dedicated state of the art models (e.g.
microphysics, LES, etc…)– Introducing stochastic events in global modelling• Toward a scientific methodology to tune
Climate models..

• Merci.
• Let’s have a great week !