Clmate ModelingClmate ModelingIn-Class Discussion:In-Class Discussion:

Constraints on Dynamic Constraints on Dynamic FluxesFluxes

VenusVenus ~ III~ III

EarthEarth ~ II, III~ II, III

MarsMars ~ I, II~ I, II

JupiterJupiter ~ I~ I

Is there a physical reason for the transition from inner to outer planets?

FOCUS HERE: JupiterFOCUS HERE: Jupiter

Dynamic Regimes of PlanetsDynamic Regimes of Planets

II III

Regime 1 => Relatively weak dynamic flux

Other energy terms in near equilibrium at all latitudes.

Max Flux vs. D: NorthMax Flux vs. D: North’’s Models Model

I

(Stone, 1978)

UseUse

ThenThen

(Equation is non-dimensional)(Equation is non-dimensional)

Recall from Lecture 15:Recall from Lecture 15:Series RepresentationsSeries Representations

Represent Q, albedo and I by series in PRepresent Q, albedo and I by series in Pnn(x)(x)

Asuume hemispheric symmetry (e.g., annual average) Asuume hemispheric symmetry (e.g., annual average)

Note: I is scaled by Qo, so that in is non-dimensional,

as is an and Sn.

Observed Series RepresentationsObserved Series Representations~ For Earth ~~ For Earth ~

Stone (1978), using Ellis & Vonder Haar (1976) data: Stone (1978), using Ellis & Vonder Haar (1976) data:

n=0 n=2 n=4

Sn 1 - 0.473 - 0.086

an 0.675 - 0.192 - 0.057

in 0.687 - 0.165 - 0.032

n=4 values < 10% of n=0 values - rapid convergence

overall accuracy (obs. and fit) is ~ 10%

aa00 + a + a22SS22/5 - i/5 - i22 = 0.693 - 0.687 = 0.006 = 0.693 - 0.687 = 0.006

(Hemispheric equilibrium, within observational accuracy)(Hemispheric equilibrium, within observational accuracy)

What might we expect for Jupiter?What might we expect for Jupiter?Why?Why?

n=0 n=2 n=4 n=6…?

Sn 1 - 0.473 (?) - 0.086 (?) ??

an - - - ??

in - - - ??

• What makes Jupiter different from Earth?What makes Jupiter different from Earth?

Structure in Jupiter's AtmosphereStructure in Jupiter's Atmosphere

n=0 n=2 n=4 n=6…?

Sn 1 - 0.473(?) - 0.086(?) ??

an - - - ??

in - - - ??

What makes Jupiter different What makes Jupiter different from Earth?from Earth?

1.1. axial tilt ~ 3˚axial tilt ~ 3˚

2.2. ……

3.3. …… (pds.jpl.nasa.gov)

UseUse

ThenThen

(Equation is non-dimensional)(Equation is non-dimensional)

Flux for Jupiter? Does It Matter?Flux for Jupiter? Does It Matter?

Represent Q, albedo and I by series in PRepresent Q, albedo and I by series in Pnn(x)(x)

Asuume hemispheric symmetry (e.g., annual average) Asuume hemispheric symmetry (e.g., annual average)

Note: I is scaled by Qo, so that in is non-dimensional,

as is an and Sn.

VenusVenus ~ III~ III

EarthEarth ~ II, III~ II, III

MarsMars ~ I, II~ I, II

JupiterJupiter ~ I~ I

Is there a physical reason for the transition from inner to outer planets?

FOCUS NOW: VenusFOCUS NOW: Venus

Dynamic Regimes of PlanetsDynamic Regimes of Planets

Dynamics Range III: D >> 1Dynamics Range III: D >> 1For D >> 1, dynamics are super-efficient:

• Temp gradients wiped out quickly, so

• T2 and hence i2 0

• Then F determined entirely by geometry of differential solar heating

F transports heat to balance differences between solar heating and infrared cooling to space.

Dynamics Range III: D >> 1Dynamics Range III: D >> 1For D >> 1, dynamics are super-efficient:

• Temp gradients wiped out quickly, so

• T2 and hence i2 0

• Then F determined entirely by geometry of differential solar heating

What makes Venus different What makes Venus different from Earth?from Earth?

1.1. axial tilt ~ 3˚axial tilt ~ 3˚

2.2. ……

3.3. ……

(www.solarviews.com)

In-Class DiscussionIn-Class Discussion

~ End ~~ End ~