understanding atmospheres across the universe atmo · across the universe atmo pascal tremblin –...
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Understandingatmospheres
acrosstheUniverse
ATMO
PascalTremblin
– 32years– 35refereedar>cles(11asfirstauthor)– 450cita>ons– Co-supervision:2PhDstudent,2masterprojects
– Exper>se:atmosphericmodeling,numerical
simula>on,HPC,comparisonwithobserva>ons
2009 2012 2015 now
PhD:CEASaclay
3Dturbulenthydrodynamics
Postdoc:Exeter
Atmosphericmodel
Permanent:MaisondelaSimula>on
HPCHydrodynamics
Forhabitabilityandbio-marker
signatureForLoca>onandprocessesfor
planetforma>on
Ø Needtocharacterizeexoplanetproper>es:• mass,radius
• pressure/temperatureprofile
• chemicalcomposi>on
Importanceofexoplanet-atmospherecharacteriza>on
ATMO–PascalTremblin 2/10
Importanceofexoplanet-atmospherecharacteriza>on
ATMO–PascalTremblin 3/10
Thermohalineconvec>oninEarth’soceans
Challenge1:
• Whydoexoplanets/Browndwarfs
emitstrongerintheinfraredthan
expected?
• Conven>onalscenariofor20years:
Clouds?
• Orfingeringconvec>oninducedby
chemicaltransi>one.g.CO/CH4?(1D
atmo:Tremblinetal.2015,2016)
Importanceofexoplanet-atmospherecharacteriza>on
ATMO–PascalTremblin 4/10
Challenge1:
• Whydoexoplanets/Browndwarfs
emitstrongerintheinfraredthan
expected?
• Conven>onalscenariofor20years:
Clouds?
• Orfingeringconvec>oninducedby
chemicaltransi>one.g.CO/CH4?(1D
atmo:Tremblinetal.2015,2016)
Challenge2:
• Whydoirradiatedexoplanetshave
inflatedradii?
• Norobustmechanismfor20years
(possiblymagne>cfields)
• Orjustcircula>onandver>cal
advec>onofpoten>altemperature?
(2Datmo:Tremblinetal.2017)
Importanceofexoplanet-atmospherecharacteriza>on
ATMO–PascalTremblin 4/10
Challenge2:
• Whydoirradiatedexoplanetshave
inflatedradii?
• Norobustmechanismfor20years
(possiblymagne>cfields?)
• Orjustcircula>onandver>cal
advec>onofpoten>altemperature?
(Tremblinetal.2017)
Ø Verypromisingbutalotofworks>llneedtobedone!
Ø Mandatorytohaverobustmodelstointerpretobserva>ons
Challenge1:
• Whydoexoplanets/Browndwarfs
emitstrongerintheinfraredthan
expected?
• Conven>onalscenariofor20years:
Clouds?
• Orfingeringconvec>oninducedby
chemicaltransi>one.g.CO/CH4?(1D
atmo:Tremblinetal.2015,2016)
UnderstandingatmospheresacrosstheUniverse
ATMO
Ø Needabecerunderstandingofthephysicalprocessespresentinatmospheres:theATMOproject
WP1:Fingeringconvec>onin
Ap/BpstarWP2:Fingeringconvec>onin
Browndwarfsandnon-
irradiatedexoplanets
WP3:Fingeringconvec>on
andcircula>onin
irradiatedexoplanets
ATMO–PascalTremblin 5/10
Small-scale
Numericalsimula>onSmall-scaletolarge-scale
Adap>veMeshRefinement
Large-scale
Globalcircula>onModel
UnderstandingatmospheresacrosstheUniverse
ATMO
Ø Needabecerunderstandingofthephysicalprocessespresentinatmospheres:theATMOproject
WP1:Fingeringconvec>onin
Ap/BpstarWP2:Fingeringconvec>onin
Browndwarfsandnon-
irradiatedexoplanets
WP3:Fingeringconvec>on
andcircula>onin
irradiatedexoplanets
ATMO–PascalTremblin 5/10
2018 2023ATMOproject
E-Elt
2025
JWSTlaunch
WP1
Fingeringconvec>oninAp/Bpstar
WP1:Ap/Bp
star
WP2:BDs/
exoplanets
WP3:Irradiated
exoplanets
Stateoftheart
• applica>onoftheboussinesqmodelof
Brownetal.(2013),Garaudetal.(2015)
Challenges
• Stra>fica>oneffect?
• Astrophysicalregime?(viscousscaletoo
small)
Newapproach
• Designanewrobusthydrodynamicsolver
forstra>fiedflow
• TakeadvantageofnewHPCarchitecture
togetclosertotheastrophysicalregime
ATMO–PascalTremblin 6/10
Appliedmathsbreakthrough(coll.S.Kokh)
• Lagrange-remapsolver
• Well-balancedforgravity
• HighorderwithMOOD
GPUs/XeonPhiwithKokkoslibrary
(Coll.P.Kestener)
PI,Postdoc1,HPCEngineer
WP2
Fingeringconvec>oninBrowndwarfsandexoplanets
WP1:Ap/Bp
star
WP2:BDs/
exoplanets
WP3:Irradiated
exoplanets
Stateoftheart
• (1D)Fingeringconvec>oninducedby
chemicalinstabili>esexplainsthespectral
reddening(Tremblinetal.2015,2016)
Challenges
• Isthe3Dturbulentenergytransport
inducedbyfingeringconvec>onefficient
enough?
• Istheextensionoftheturbulentzonebig
enough?
Newapproach
• UseAdapta>veMeshRefinementto
resolvethesmallscalefingersandthe
extensionoftheturbulentregion
• Dynamicalstudyandparametriza>onof
chemicalinstabili>esfor1Dmodel
ATMO–PascalTremblin 7/10
PI,PhD1,HPCEngineer
Preliminaryresultof
thedynamicalCO/CH4
instability
WP3
Fing.convec>onandcircula>oninirradiatedexoplanets
WP1:Ap/Bp
star
WP2:BDs/
exoplanets
WP3:Irradiated
exoplanets
Stateoftheart
• 2Dsteadystatecircula>onmodelexpains
theinflatedradii(Tremblinetal.2017)
Challenges
• Whataboutthe3Dsteadycircula>on?
• Andtheinterplaywithfing.convec>on?
Newapproach
• Usetheefficencyofrecentcircula>on
model(Dynamico)toreachthe3Dsteady
state
• Studyfingeringconvec>oninaforced
shearflowboxmodel,extensionofthe
parametriza>onforglobalmodels
ATMO–PascalTremblin 8/10
PI,PhD2,HPCEngineer
Scalingofthenew
cirula>onmodel
Dynamico
WP1:Ap/Bp
star
WP2:BDs/
exoplanets
WP3:Irradiated
exoplanets
ATMO–PascalTremblin 9/10
UnderstandingatmospheresacrosstheUniverse
ATMO
LowestrisksWP2/3:
• Parametriza>onoftheinstability
• Implementa>oninglobal1D/3D
atmosphericmodels
HighestrisksWP1:
stra>fiedhydro-solver
• Lagrange-remap->low-machsolver
• Well-balancedgravity->relaxa>on
• HighorderMOOD->2ndorderscheme
WP1:Ap/Bp
star
WP2:BDs/
exoplanets
WP3:Irradiated
exoplanets
ATMO–PascalTremblin
UnderstandingatmospheresacrosstheUniverse
ATMO
10/10
2018 2023ATMOproject
E-Elt
2025
JWSTlaunch
Team:Posdoc1,PhD1,PhD2
PI,HPCEngineer
(Hostins>tute:CEASalcay)
Budget:
Manpower(60%),HPCinvestments(11%)
Travel,publica>ons(9%)Overheads(20%)
Deliverables
• Aninnova>vesolverforstra>fied
hydrodynamics
• Parametriza>onoffingering
convec>onforglobalmodels
• Produceexoplanetsspectra,phase
curvesforfutureJWST/E-elt
observa>ons(PIassociatedtoMIRI
consor>um)
Transferinotherfields
• Applica>onofthesolverfor
oceanicdynamics
�2.0 �1.5 �1.0 �0.5 0.0 0.5 1.0 1.5 2.0
J-H band Color
10
15
20
25
Jba
ndM
agni
tude
Stars
Brown Dwarfs
Exoplanets
Importanceofexoplanet-atmospherecharacteriza>on
?
models
«red»spectra
ATMO–PascalTremblin 4/10
Whydoexoplanets/Browndwarfsemit
strongerintheinfraredthanexpected?
�2.0 �1.5 �1.0 �0.5 0.0 0.5 1.0 1.5 2.0
J-H band Color
10
15
20
25
Jba
ndM
agni
tude
Stars
Brown Dwarfs
Exoplanets
Importanceofexoplanet-atmospherecharacteriza>on
?
models
«red»spectra
ATMO–PascalTremblin 4/10
Whydoexoplanets/Browndwarfsemit
strongerintheinfraredthanexpected?
Clouds?
orfingeringconvec>on?
(Tremblinetal.2015,2016)
�2.0 �1.5 �1.0 �0.5 0.0 0.5 1.0 1.5 2.0
J-H band Color
10
15
20
25
Jba
ndM
agni
tude
Stars
Brown Dwarfs
Exoplanets
Importanceofexoplanet-atmospherecharacteriza>on
?
models
«red»spectra
ATMO–PascalTremblin 4/10
Whydoexoplanets/Browndwarfsemit
strongerintheinfraredthanexpected?
Clouds?
orfingeringconvec>on?
(Tremblinetal.2015,2016)
models
?Inflatedradii
Whydoirradiatedexoplanetshave
inflatedradii?
�2.0 �1.5 �1.0 �0.5 0.0 0.5 1.0 1.5 2.0
J-H band Color
10
15
20
25
Jba
ndM
agni
tude
Stars
Brown Dwarfs
Exoplanets
Importanceofexoplanet-atmospherecharacteriza>on
?
models
«red»spectra
ATMO–PascalTremblin 4/10
Whydoexoplanets/Browndwarfsemit
strongerintheinfraredthanexpected?
Clouds?
orfingeringconvec>on?
(Tremblinetal.2015,2016)
models
?Inflatedradii
Whydoirradiatedexoplanetshave
inflatedradii?
Magne>cfields?
orcircula>on?
(Tremblinetal.2017)