hydrodynamical simulations of strongly irradiated...
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![Page 1: Hydrodynamical Simulations of Strongly Irradiated Planetsonline.itp.ucsb.edu/online/exoplanets10/dobbsdixon/pdf/... · 2010. 2. 2. · Sagan Postdoctoral Fellow Nick Cowan Hemispherically](https://reader036.vdocuments.mx/reader036/viewer/2022071514/6135204bdfd10f4dd73c2c04/html5/thumbnails/1.jpg)
Ian Dobbs-Dixon, UW SeattleSagan Postdoctoral Fellow
Hydrodynamical Simulations ofStrongly Irradiated Planets
Ian Dobbs-DixonSagan Postdoctoral FellowUniversity of Washington
![Page 2: Hydrodynamical Simulations of Strongly Irradiated Planetsonline.itp.ucsb.edu/online/exoplanets10/dobbsdixon/pdf/... · 2010. 2. 2. · Sagan Postdoctoral Fellow Nick Cowan Hemispherically](https://reader036.vdocuments.mx/reader036/viewer/2022071514/6135204bdfd10f4dd73c2c04/html5/thumbnails/2.jpg)
Ian Dobbs-Dixon, UW SeattleSagan Postdoctoral Fellow
Dynamical Methods• Equivalent Barotropic and Shallow Water (2D)
– Cho et al (2003,2008) Langton and Laughlin (2007,2008)Rauscher et al (2007, 2008)
• Primitive equations (~3D)– Showman et al. (2002, 2005, 2006, 2008, 2009), Menou
and Rauscher (2009)• Navier-Stokes equation (2D)
– Burkert et al. 2007• Full Navier-Stokes equations (3D)
– Dobbs-Dixon et al (2008,2009)
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Ian Dobbs-Dixon, UW SeattleSagan Postdoctoral Fellow
Radiation Transfer Methods• Relaxation methods (Newtonian heating)
– Cho et al (2003,2008) Langton and Laughlin (2007,2008) Rauscher etal (2007, 2008), Showman et al. (2002, 2005, 2006, 2008), Menou andRauscher (2009)
• 2/3D one temperature flux-limited radiative diffusion– Burkert et al. (2007), Dobbs-Dixon and Lin (2008)
• 3D FLD + decoupled thermal and radiative components– Dobbs-Dixon et al (2009)
• 1D (radial) wavelength-dependent radiative transfer– Showman et al. (2009)
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Ian Dobbs-Dixon, UW SeattleSagan Postdoctoral Fellow
3D Navier-Stokes, flux limited diffusion anddecoupled thermal and radiative components
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Ian Dobbs-Dixon, UW SeattleSagan Postdoctoral Fellow
Absorption vs. EmissionOpacities
(κ*/κ
P)1
/4
T (K)
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Ian Dobbs-Dixon, UW SeattleSagan Postdoctoral Fellow
Prot=Porb=3.52d, Tstar=6117K
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Ian Dobbs-Dixon, UW SeattleSagan Postdoctoral Fellow
Photospheric Velocities
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Ian Dobbs-Dixon, UW SeattleSagan Postdoctoral Fellow
HD209458b
anti-solar
sub-solar
Tem
pera
ture
(K)
Pressure (bar) Burrows et al (2007)
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Ian Dobbs-Dixon, UW SeattleSagan Postdoctoral Fellow
ν
1012cm2/s
108cm2/s
1010cm2/s
Velocity Structure
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Ian Dobbs-Dixon, UW SeattleSagan Postdoctoral Fellow
Temperature Structure
ν
1012cm2/s
108cm2/s
1010cm2/s
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Ian Dobbs-Dixon, UW SeattleSagan Postdoctoral Fellow
Variability
Grillmair et al 2009 Agol et al 2008
Madhusudhan and Seager 2009
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Ian Dobbs-Dixon, UW SeattleSagan Postdoctoral Fellow
Ian Dobbs-Dixon, University of Washington,Seattle, WA
To To+0.5d
To+1.0d To+1.5d
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Ian Dobbs-Dixon, UW SeattleSagan Postdoctoral Fellow
Surface and radial shear
T (K)vφ
+4 km/s-4 km/s
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Ian Dobbs-Dixon, UW SeattleSagan Postdoctoral Fellow
Nick Cowan
Hemispherically averaged phase curves(approximate )
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Ian Dobbs-Dixon, UW SeattleSagan Postdoctoral Fellow
Transmission SpectraEgress SpectraFull Disk Spectra
Beaulieu (2008)
Opacities fromSharp and Burrows (2007)
H20 opacities fromBarber et al (2006)
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Ian Dobbs-Dixon, UW SeattleSagan Postdoctoral Fellow
Viscous Variations
V5, whole disk V5 western V5 eastern
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Ian Dobbs-Dixon, UW SeattleSagan Postdoctoral Fellow
Conclusions• Numerical treatment of radiation and dynamics must be
included as coupled model• Opacity and dynamical temperature inversions play roles in
dynamics and spectra• Three quasi-jets (one equatorial and two mid-lat.) are common
features, with width decreasing with increased planetary rotationperiod
• Optical and IR opacities both are important in determininglocation of stellar energy deposition and efficiency ofredistribution to the night-side
• Changing viscosity drastically alters streamlines, changingoverall thermal structure
• Dynamically driven variability may cause variations transitspectra, but variation in hemispherically averaged phase curveswill be difficult