1 / 17

The Interplay Between a Hot Jupiter's Thermal Evolution and its Atmospheric Circulation

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. Arras & Bildsten (2006). Guillot & Showman (2002).

tobias
Download Presentation

The Interplay Between a Hot Jupiter's Thermal Evolution and its Atmospheric Circulation

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. The Interplay Between a Hot Jupiter's Thermal Evolution and its Atmospheric Circulation Emily Rauscher1,2 Adam Showman1 1University of Arizona 2NASA Sagan Fellow

  2. Rauscher The radiative-convective boundary and the cooling rate Arras & Bildsten (2006) Guillot & Showman (2002)

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

  4. Rauscher Model set-up same dynamics as Rauscher & Menou 2010, new radiative transfer

  5. Rauscher Rauscher & Menou, in prep The code Double-gray

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

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

  8. The code Rauscher Rauscher & Menou, in prep analytic solution from Guillot (2010),see also Hansen (2008)

  9. Rauscher A range of internal heat fluxes Globally averaged profiles Sub- and anti-stellar profiles PRCB at 130, 50, and 20 bar.

  10. Rauscher Preliminary results

  11. Preliminary Rauscher Average wind speeds

  12. Preliminary Rauscher Zonal wind structure Tint=125 K Tint=350 K Tint=500 K Tint=1000 K Tint=1410 K Tint=2000 K

  13. Preliminary Rauscher Temperature and wind maps at 1 bar Tint=125 K Tint=1000 K Tint=1410 K Tint=2000 K

  14. Preliminary Rauscher Temperature and wind maps at 150 bar Tint=500 K Tint=1000 K Tint=1410 K Tint=2000 K

  15. Preliminary Rauscher 2-D radiative-convective boundary Tint=1000 K Tint=1410 K PRCB,min= 75 bar PRCB,min= 13 bar Tint=2000 K PRCB,min= 9 bar

  16. Preliminary Rauscher Efficiency of downward transport of E downward kinetic energy incident stellar heating =

  17. Rauscher 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%

More Related