The Interplay Between a Hot Jupiter's Thermal Evolution and its Atmospheric Circulation Emily Rauscher 1,2 Adam Showman 1 1 University of Arizona 2 NASA.

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Presentation transcript:

The Interplay Between a Hot Jupiter's Thermal Evolution and its Atmospheric Circulation Emily Rauscher 1,2 Adam Showman 1 1 University of Arizona 2 NASA Sagan Fellow

The radiative-convective boundary and the cooling rate Guillot & Showman (2002) 9/13/11Rauscher Arras & Bildsten (2006)

Downward transport of kinetic energy? Showman & Guillot (2002) 9/13/11Rauscher Efficiency = (downward KE)/(incident flux) ≈ 1%

same dynamics as Rauscher & Menou 2010, new radiative transfer 9/13/11Rauscher

The code 9/13/11Rauscher Rauscher & Menou, in prep Double-gray

9/13/11Rauscher The code 9/13/11Rauscher Rauscher & Menou, in prep Double-gray Infrared absorption coefficient increases with pressure

9/13/11Rauscher The code 9/13/11Rauscher Rauscher & Menou, in prep Double-gray Infrared absorption coefficient increases with pressure At high optical depths transition to diffusion approximation for radiative flux

9/13/11Rauscher The code Rauscher & Menou, in prep analytic solution from Guillot (2010), see also Hansen (2008)

A range of internal heat fluxes Globally averaged profiles P RCB at 130, 50, and 20 bar. 9/13/11Rauscher Sub- and anti-stellar profiles

9/13/11Rauscher

Average wind speeds 9/13/11Rauscher Preliminary

Zonal wind structure 9/13/11Rauscher T int =125 KT int =350 KT int =500 K T int =2000 KT int =1000 KT int =1410 K Preliminary

Temperature and wind maps at 1 bar 9/13/11Rauscher Preliminary T int =1000 KT int =1410 KT int =2000 K T int =125 K

T int =1000 KT int =1410 KT int =2000 K Temperature and wind maps at 150 bar 9/13/11Rauscher T int =500 K Preliminary

2-D radiative-convective boundary 9/13/11Rauscher P RCB,min = 75 barP RCB,min = 13 bar P RCB,min = 9 bar T int =1000 KT int =1410 K T int =2000 K Preliminary

Efficiency of downward transport of E 9/13/11Rauscher Preliminary downward kinetic energy incident stellar heating =

Summary We see changes in the circulation across a range of internal heat fluxes The location of the radiative-convective boundary is 2-D and complex (and requires further analysis) The (preliminary) efficiencies we are finding are low, < 0.12% 9/13/11Rauscher

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