Understanding atmospheres across the Universe ATMO
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1 Understanding atmospheres across the Universe ATMO 32 years Pascal Tremblin 35 refereed ar>cles (11 as first author) 450 cita>ons Co-supervision: 2 PhD student, 2 master projects Exper>se: atmospheric modeling, numerical simula>on, HPC, comparison with observa>ons now PhD: CEA Saclay 3D turbulent hydrodynamics Postdoc: Exeter Atmospheric model Permanent: Maison de la Simula>on HPC Hydrodynamics
2 Importance of exoplanet-atmosphere characteriza>on For habitability and bio-marker signature For Loca>on and processes for planet forma>on Ø Need to characterize exoplanet proper>es: mass, radius pressure/temperature profile chemical composi>on ATMO Pascal Tremblin 2/10
3 Importance of exoplanet-atmosphere characteriza>on Challenge 1: Why do /Brown dwarfs emit stronger in the infrared than expected? Conven>onal scenario for 20 years: Clouds? Or fingering convec>on induced by chemical transi>on e.g. CO/CH4? (1D atmo: Tremblin et al. 2015,2016) Thermohaline convec>on in Earth s oceans ATMO Pascal Tremblin 3/10
4 Importance of exoplanet-atmosphere characteriza>on Challenge 1: Why do /Brown dwarfs emit stronger in the infrared than expected? Conven>onal scenario for 20 years: Clouds? Or fingering convec>on induced by chemical transi>on e.g. CO/CH4? (1D atmo: Tremblin et al. 2015,2016) Challenge 2: Why do irradiated have inflated radii? No robust mechanism for 20 years (possibly magne>c fields) Or just circula>on and ver>cal advec>on of poten>al temperature? (2D atmo: Tremblin et al. 2017) ATMO Pascal Tremblin 4/10
5 Importance of exoplanet-atmosphere characteriza>on Challenge 1: Why do /Brown dwarfs emit stronger in the infrared than expected? Conven>onal scenario for 20 years: Clouds? Or fingering convec>on induced by chemical transi>on e.g. CO/CH4? (1D atmo: Tremblin et al. 2015,2016) Challenge 2: Why do irradiated have inflated radii? No robust mechanism for 20 years (possibly magne>c fields?) Or just circula>on and ver>cal advec>on of poten>al temperature? (Tremblin et al. 2017) Ø Very promising but a lot of work s>ll need to be done! Ø Mandatory to have robust models to interpret observa>ons ATMO Pascal Tremblin 4/10
6 Understanding atmospheres across the Universe ATMO Ø Need a becer understanding of the physical processes present in atmospheres: the ATMO project WP1: Fingering convec>on in Ap/Bp star WP2: Fingering convec>on in Brown dwarfs and nonirradiated WP3: Fingering convec>on and circula>on in irradiated Small-scale Numerical simula>on Small-scale to large-scale Adap>ve Mesh Refinement Large-scale Global circula>on Model ATMO Pascal Tremblin 5/10
7 Understanding atmospheres across the Universe ATMO Ø Need a becer understanding of the physical processes present in atmospheres: the ATMO project WP1: Fingering convec>on in Ap/Bp star WP2: Fingering convec>on in Brown dwarfs and nonirradiated WP3: Fingering convec>on and circula>on in irradiated ATMO project JWST launch 2025 E-Elt ATMO Pascal Tremblin 5/10
8 WP1 Fingering convec>on in Ap/Bp star State of the art applica>on of the boussinesq model of Brown et al. (2013), Garaud et al. (2015) WP1: Ap/Bp star WP2: BDs/ WP3: Irradiated Challenges Stra>fica>on effect? Astrophysical regime? (viscous scale too small) PI, Postdoc1, HPC Engineer New approach Design a new robust hydrodynamic solver for stra>fied flow Take advantage of new HPC architecture to get closer to the astrophysical regime Applied maths breakthrough (coll. S. Kokh) Lagrange-remap solver Well-balanced for gravity High order with MOOD GPUs/Xeon Phi with Kokkos library (Coll. P.Kestener) ATMO Pascal Tremblin 6/10
9 WP2 Fingering convec>on in Brown dwarfs and State of the art (1D) Fingering convec>on induced by chemical instabili>es explains the spectral reddening (Tremblin et al. 2015,2016) Challenges Is the 3D turbulent energy transport induced by fingering convec>on efficient enough? WP1: Ap/Bp star WP2: BDs/ WP3: Irradiated Is the extension of the turbulent zone big enough? New approach Use Adapta>ve Mesh Refinement to resolve the small scale fingers and the extension of the turbulent region Dynamical study and parametriza>on of chemical instabili>es for 1D model PI, PhD1, HPC Engineer Preliminary result of the dynamical CO/CH4 instability ATMO Pascal Tremblin 7/10
10 WP3 Fing. convec>on and circula>on in irradiated State of the art 2D steady state circula>on model expains the inflated radii (Tremblin et al. 2017) WP1: Ap/Bp star WP2: BDs/ WP3: Irradiated Challenges What about the 3D steady circula>on? And the interplay with fing. convec>on? New approach Use the efficency of recent circula>on model (Dynamico) to reach the 3D steady state Study fingering convec>on in a forced shear flow box model, extension of the parametriza>on for global models PI, PhD2, HPC Engineer Scaling of the new cirula>on model Dynamico ATMO Pascal Tremblin 8/10
11 Understanding atmospheres across the Universe ATMO Highest risks WP1: stra>fied hydro-solver WP1: Ap/Bp star WP2: BDs/ WP3: Irradiated Lagrange-remap -> low-mach solver Well-balanced gravity -> relaxa>on High order MOOD -> 2 nd order scheme Lowest risks WP2/3: Parametriza>on of the instability Implementa>on in global 1D/3D atmospheric models ATMO Pascal Tremblin 9/10
12 Understanding atmospheres across the Universe ATMO Deliverables An innova>ve solver for stra>fied hydrodynamics WP1: Ap/Bp star WP2: BDs/ WP3: Irradiated Parametriza>on of fingering convec>on for global models Produce spectra, phase curves for future JWST/E-elt observa>ons (PI associated to MIRI consor>um) Team: Posdoc1, PhD1, PhD2 PI, HPC Engineer (Host ins>tute: CEA Salcay) Transfer in other fields Applica>on of the solver for oceanic dynamics ATMO project JWST launch Budget: Manpower (60%), HPC investments (11%) Travel, publica>ons (9%) Overheads (20%) 2025 E-Elt ATMO Pascal Tremblin 10/10
13 Importance of exoplanet-atmosphere characteriza>on Why do /Brown dwarfs emit stronger in the infrared than expected? Stars 10 Brown Dwarfs models Exoplanets JbandMagnitude 15? «red» spectra J-H band Color ATMO Pascal Tremblin 4/10
14 Importance of exoplanet-atmosphere characteriza>on Why do /Brown dwarfs emit stronger in the infrared than expected? Stars 10 Brown Dwarfs models Exoplanets JbandMagnitude 15 20? Clouds? or fingering convec>on? (Tremblin et al. 2015,2016) 25 «red» spectra J-H band Color ATMO Pascal Tremblin 4/10
15 Importance of exoplanet-atmosphere characteriza>on Why do /Brown dwarfs emit stronger in the infrared than expected? Stars Why do irradiated have inflated radii? 10 Brown Dwarfs models JbandMagnitude 15 20? Exoplanets Clouds? or fingering convec>on? (Tremblin et al. 2015,2016) Inflated radii? models 25 «red» spectra J-H band Color ATMO Pascal Tremblin 4/10
16 Importance of exoplanet-atmosphere characteriza>on Why do /Brown dwarfs emit stronger in the infrared than expected? Stars Why do irradiated have inflated radii? 10 Brown Dwarfs models JbandMagnitude 15 20? Exoplanets Clouds? or fingering convec>on? (Tremblin et al. 2015,2016) Inflated radii? Magne>c fields? or circula>on? (Tremblin et al. 2017) models 25 «red» spectra J-H band Color ATMO Pascal Tremblin 4/10
Understanding atmospheres across the Universe ATMO
PI: Pascal Tremblin Understanding atmospheres across the Universe ATMO Host Ins
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