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Understanding Dynamic Fluxes and Regimes of Inner vs. Outer Planets: A Comparative Analysis

This discussion explores the dynamic regimes of terrestrial and gas giant planets, focusing on the variations in fluxes, energy equilibrium, and atmospheric structures of Venus, Earth, Mars, and Jupiter. It evaluates the physical reasons for the transition between inner and outer planets, emphasizing models from Stone (1978) and observed series representations. Key elements include axial tilts, temperature gradients, and the implications of super-efficient dynamics, particularly in Venus and Jupiter. Insights gained can deepen our understanding of planetary climate systems and their unique characteristics.

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Understanding Dynamic Fluxes and Regimes of Inner vs. Outer Planets: A Comparative Analysis

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  1. Clmate Modeling In-Class Discussion: Constraints on Dynamic Fluxes

  2. Dynamic Regimes of Planets Venus ~ III Earth ~ II, III Mars ~ I, II Jupiter ~ I Is there a physical reason for the transition from inner to outer planets? FOCUS HERE: Jupiter

  3. Max Flux vs. D: North’s Model III I II (Stone, 1978) Regime 1 => Relatively weak dynamic flux Other energy terms in near equilibrium at all latitudes.

  4. Recall from Lecture 15:Series Representations Represent Q, albedo and I by series in Pn(x) Asuume hemispheric symmetry (e.g., annual average) Note: I is scaled by Qo, so that in is non-dimensional, as is an and Sn. Use Then (Equation is non-dimensional)

  5. Observed Series Representations~ For Earth ~ 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% a0 + a2S2/5 - i2 = 0.693 - 0.687 = 0.006 (Hemispheric equilibrium, within observational accuracy)

  6. What might we expect for Jupiter?Why? n=0 n=2 n=4 n=6…? Sn 1 - 0.473 (?) - 0.086 (?) ?? an - - - ?? in - - - ?? • What makes Jupiter different from Earth?

  7. Structure in Jupiter's Atmosphere n=0 n=2 n=4 n=6…? Sn 1 - 0.473(?) - 0.086(?) ?? an - - - ?? in - - - ?? What makes Jupiter different from Earth? axial tilt ~ 3˚ … … (pds.jpl.nasa.gov)

  8. Flux for Jupiter? Does It Matter? Represent Q, albedo and I by series in Pn(x) Asuume hemispheric symmetry (e.g., annual average) Note: I is scaled by Qo, so that in is non-dimensional, as is an and Sn. Use Then (Equation is non-dimensional)

  9. Dynamic Regimes of Planets Venus ~ III Earth ~ II, III Mars ~ I, II Jupiter ~ I Is there a physical reason for the transition from inner to outer planets? FOCUS NOW: Venus

  10. Dynamics Range III: D >> 1 • For 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.

  11. Dynamics Range III: D >> 1 • For 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 from Earth? axial tilt ~ 3˚ … … (www.solarviews.com)

  12. In-Class Discussion~ End ~

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