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 Interplay Between a Hot Jupiter's Thermal Evolution and its Atmospheric Circulation
Feb 22, 2016
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). - PowerPoint PPT Presentation
Welcome message from author
This document is posted to help you gain knowledge. Please leave a comment to let me know what you think about it! Share it to your friends and learn new things together.
Transcript
The Interplay Between a Hot Jupiter's Thermal Evolution and its Atmospheric CirculationEmily Rauscher1,2
Adam Showman1
1University of Arizona2NASA Sagan Fellow
Rauscher
The radiative-convective boundary and the cooling rate
Guillot & Showman (2002)
9/13/11
Arras & Bildsten (2006)
Rauscher
Downward transport of kinetic energy?
Showman & Guillot (2002)
9/13/11
Efficiency = (downward KE)/(incident flux)
≈ 1%
Rauscher
Model set-upsame dynamics as Rauscher & Menou 2010, new radiative transfer
9/13/11
RauscherThe code 9/13/11
Rauscher & Menou, in prep
Double-gray
Rauscher 9/13/11The code 9/13/11Rauscher
Rauscher & Menou, in prep
Double-gray
Infrared absorption coefficient increases with
pressure
Rauscher 9/13/11The 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
Rauscher 9/13/11The code Rauscher & Menou, in prep
analytic solution from Guillot (2010),see also Hansen (2008)
Rauscher
A range of internal heat fluxesGlobally averaged profiles
PRCB at 130, 50, and 20 bar.
9/13/11
Sub- and anti-stellar profiles
Rauscher
Preliminary results
9/13/11
Rauscher
Average wind speeds9/13/11
Preliminary
RauscherZonal wind structure 9/13/11
Tint=125 K Tint=350 K Tint=500 K
Tint=2000 K
Tint=1000 K
Tint=1410 K
Preliminary
Rauscher
Temperature and wind maps at 1 bar9/13/11
Preliminary
Tint=1000 K
Tint=1410 K
Tint=2000 K
Tint=125 K
Rauscher
Tint=1000 K
Tint=1410 K
Tint=2000 K
Temperature and wind maps at 150 bar9/13/11
Tint=500 K
Preliminary
Rauscher2-D radiative-convective boundary
9/13/11
PRCB,min = 75 bar PRCB,min = 13 bar
PRCB,min = 9 bar
Tint=1000 K
Tint=1410 K
Tint=2000 K
Preliminary
Rauscher
Efficiency of downward transport of E9/13/11
Preliminary
downward kinetic energyincident stellar heating=
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%
9/13/11
Related Documents
