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Planetary Engineering 1

This exercise focuses on the global energy balance and radiative equilibrium essential for understanding planetary temperatures. We explore how temperature (Trad) changes with distance from the Sun, emphasizing that the solar flux decreases with distance squared. Using data on various planets, we analyze factors like distance, albedo, and outgoing IR to calculate Trad. The goal is to assess how we might alter surface temperatures on planets like Mars and Mercury while recognizing the challenges posed by planets like Venus.

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Planetary Engineering 1

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  1. Planetary Engineering 1 Climate Modeling Class Exercise

  2. Zero-Dimensional GEBM Global energy balance: Radiative equilibrium (in = out)

  3. Goal: Planets’ Temperatures Important Fact: Sun heats less the farther it is. Important Factor: How does S change with orbit?

  4. Recall from Topic 1: Change in solar flux: sun  earth At photosphere surface, solar flux ~ 6.2.107 W-m-2 At Earth’s orbit, solar flux ~ 1360 W-m-2

  5. Two Spheres Surrounding Sun Total energy flux the same through each sphere R2 = 2 x R1 R2 R1 The same area at R2 intercepts only 1/4 of energy it intercepts at R1  Flux decreases as R-2

  6. For Earth Global energy balance: Radiative equilibrium (in = out) Thus, TRAD= 255 K

  7. What about other planets? How does Trad change with orbit?

  8. What about other planets? How does Trad change with orbit? Planet Distance Albedo Outgoing IR Trad from sun [A.U.] [W-m2] [K] Mercury 0.39 0.06 Venus 0.72 0.76 Earth 1.00 0.30 238 255 Mars 1.52 0.16 Jupiter 5.20 0.51 Saturn 9.54 0.50 Uranus 19.18 0.66 Neptune 30.06 0.62

  9. For Mars Tsurface ≈ Trad. How warm can we make its surface?

  10. For Mercury Tsurface ≈ Trad. How cool can we make its surface?

  11. Venus? Why can’t we adjust Venus the same way?

  12. End Planetary Engineering 1

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