To calculate the equilibrium temperature of the Earth, we use the following formula for a planet's equilibrium temperature:

$T_e = \left( \frac{(1 - A) \cdot S}{4 \cdot \sigma} \right)^{\frac{1}{4}}$

Where:

• $T_e$ is the equilibrium temperature (in Kelvin).
• $A$ is the albedo (dimensionless).
• $S$ is the solar constant (in $W/m^2$).
• $\sigma$ is the Stefan-Boltzmann constant, which is $5.67 \times 10^{-8} \, W/m^2K^4$.

Given values:

• Albedo $A = 0.80$
• Solar constant $S = 1361 \, W/m^2$

Now let's calculate:

$T_e = \left( \frac{(1 - 0.80) \cdot 1361}{4 \cdot 5.67 \times 10^{-8}} \right)^{\frac{1}{4}}$

First, simplify the expression step-by-step.

I'll compute that for you.The calculated equilibrium temperature of the Earth, based on the given values, is approximately 186 K (rounded to the nearest whole number).

Would you like further details on this calculation or have any additional questions?

Here are five related questions:

1. How does Earth's albedo affect its equilibrium temperature?
2. What is the significance of the solar constant in climate studies?
3. How does the actual observed surface temperature compare to the equilibrium temperature?
4. What factors could cause the equilibrium temperature to differ from the observed surface temperature?
5. How would a change in Earth's distance from the Sun affect the equilibrium temperature?

Tip: The equilibrium temperature is an approximation that assumes no atmosphere. Adding the greenhouse effect raises the actual surface temperature.