CHARACTERIZING EXOPLANET ATMOSPHERES USING GENERAL CIRCULATION MODELS Tiffany Kataria 3 July, 5 With thanks to collaborators David Sing, Adam Showman, Hannah Wakeford, Thomas Evans, Nikolay Nikolov, Jonathan Fortney, Mark Marley, Kevin Stevenson, Nikole Lewis
INTRODUCTION Exoplanet circulation modelling Allows us to probe dynamical regimes beyond our own solar system, which expands our overall knowledge of atmospheric dynamics Provides insights to three-dimensional structure Temperature, heating/cooling rates, composition, clouds, chemistry Complements -D models in interpreting observations of exoplanet atmospheres: transmission/emission spectra, phase curves, eclipse maps Now that we have a (relatively) large observational dataset for a range of planets over a large wavelength range, we can identify trends in atmospheric properties and conduct detailed comparative studies
SAMPLE STUDIES WASP-43b, an ultra-short period hot Jupiter Dataset: Spectrophotometric phase curves with HST/WFC3 Objectives: Place constraints on atmospheric metallicity Large HST program, hot Jupiters observed in transmission Dataset: Transmission spectra of HJs with STIS and WFC3 Objectives: Understand role of clouds on target sample 55 Cnc e, an ultra-short period super Earth Dataset: Spitzer transit/eclipse measurements from -3 Objectives: Constrain composition and atmospheric variability
COMPARING GCMS TO SPECTROPHOTOMETRIC DATA: WFC3 OBSERVATIONS OF WASP-43B Kataria et al. 5 DAYSIDE EMISSION SPECTRUM WHITE LIGHT PHASE CURVE
COMPARISON TO HST WFC3 OBSERVATIONS SPECTROPHOTOMETRIC PHASE CURVES Red: x solar model Blue: 5x solar model Kataria et al. (5)
COMPARISON TO HST WFC3 OBSERVATIONS EMISSION SPECTRA Red: x solar model Blue: 5x solar model Kataria et al. (5)
HST LARGE PROGRAM STUDY Cloudy versus cloud-free planets Huitson et al. 3; Wakeford et al. 3; Sing et al. 3, 5; Nikolov et al. 4, 5; Ballester et al. in prep
8µm ingress and egress of HD 89733b..4.. -. -.6 -.4 -. -. Orbital Phase..4 IRAC Ch WFC3.4 WFC3 -.4 -... -. Orbital Phase..4.6. -..4. Planet/Star Flux Relative Flux Ultra-short period (~9 hr) planet with a wide array of observational constraints -.. -.6.6.8.6 WASP-9b IRAC Ch Relative Flux Relative Flux.6 Relative Flux.8 Figure : (from Majeau et al. ()) Schematic demonstration.8 IRAC of Ch eclipse mapping, which creates two orthogonal scans of the planet s.6 dayside during eclipse ingress and.4 egress. The bottom panels shows the brightness maps derived from the. 8µm ingress and egress of.4. HD 89733b. -.4. -....3 Orbital phase.4.5. -. -. -.6 -.4 -.4 -. -. Orbital Phase..4.6 Preliminary reductions by N. K. Lewis and C. M. Huitson
DISENTANGLING CLOUDS D radiative equilibrium PT profiles from Jonathan Fortney
6 HD 89733b, x solar, 5 days 6 6 35 5 3 8 5 34 3 8648 6 3 4 36 34 3 3 8 6 8 6 4 6 4 38 4 5 6 5 6 8 5 (m s ) 8 6 8 6 6 4 4 6 8 6 5 58 6 54 5 46 4 38 34 3 6 8 4 6 4 6 3 (m s ) 5 3 8 6 4 6 4 8 4 56 54 5 5 48 46 8 4 8 44 6 8 4 46 6 4 4 3 6 4 8 8 38 3 6 44 8 4 43 4 38 36 34 4 4 6 4 8 84 34 36 8 WASP 9b, x solar 34 46 8 6 4 5 8 3 4 5 (m s ) 8 4 3 5 3 6 8 6 35 8 6 (m s ) 4 4 8 6 4 38 4 6 36 3 3 8 34 6 4 8 6 4 3 3 5 45 4 8 6 86 4 4 8 WASP 7b, x solar 6 4 5 6 6 8 8 6 4 3 6 5 8 5 (m s ) 8 6 4 4 4 6 34 5 5 6 WASPb, x solar 6 5 3 4 8 4 8 4 4 6 6 8 6 6 35 8 8 HD9, x solar 8 5 6 5 6 8 4 (m s ) 8 6 4 8 6 4 8 6 5 4 4 6 HAT P b, x solar 6 4 8 (m s ) 8 5 4 3 8 8 6 8 6 4 4 6 6 6 4 8 4 4 8 8 4 6 5 8 6 5 5 4 4 4 4 8 6 8 6 5 3 4 4 8 8 6 4 8 6 8 5 4 6 4 6 8 8 6 6 8 4 5 5 6 8 4 4 6 6 8 4 4 8 5 4 6 5 8 5 WASP9b, x solar WASP 6b, x solar 4 4 HAT P b, x solar 4 6 8 (m s ) 8 6 4 6 8 (m s )
Figure : Wind/temperature profile at mbar. HAT P b, x solar, 5.4 mbar WASP 6b, x solar, 5.4 mbar WASP9b, x solar, 5.4 mbar 8 6 4 8 6 4 8 6 4 3 9 8 9 6 8 5 5 5 5 7 6 6 8 5 5 5 5 8 7 6 8 5 5 5 5 9 8 HD 89733b, x solar, 3.95 mbar HAT P b, x solar, 5.4 mbar HD9, x solar, 5.4 mbar 8 6 4 6 8 5 5 5 5 3 9 8 7 8 6 4 6 8 5 5 5 5 4 3 8 6 4 6 8 5 5 5 5 6 5 4 3 WASPb, x solar, 5.4 mbar WASP 7b, x solar, 5.4 mbar WASP 9b, x solar,. mbar 8 6 4 6 8 5 5 5 5 9 8 7 6 5 4 3 8 6 4 6 8 5 5 5 5 8 6 4 8 6 4 6 8 5 5 5 5 8 6 4 8 6 4
VARIABILITY ON 55 Cnc e? 3 Occultation depth [ppm] 5 5 5 Transit depth [ppm] 6 5 4 3 55 56 57 58 594 5947 5954 596 645 6467 6483 65 Time [BJD-,45,] Demory et al. 5
TEMPORAL VARIABILITY 5x solar Normalized Secondary Eclipse Depth...998.996 4 7 3...998 H O-dominated.996 4 75 8 4 CO -dominated...998.996 55 45 9 Time (Earth days)
CONCLUSIONS AND FUTURE WORK Three-dimensional circulation models can be used to lend insights on a variety of observational datasets, and help answer fundamental questions about their atmospheric properties GCM-derived models can provide constraints, but they re not perfect For example, model phase curves generally over-predict nightside flux Enhancement of C/O ratio, disequilibrium chemistry, and/or clouds can be invoked to explain discrepancy, but detailed models are needed to explore these effects Need GCMs that encapsulate more complex physics However, with great complexity comes great responsibility Idealized models help identify fundamental dynamical mechanisms