Estimating the Equilibrium Temperature of Planets

This short video demonstrates how astrophysicists can use the Stefan-Boltzman equation for a spherical object emitting thermal (black body) radiation, to estimate the equillibrium temperature of planets, or other spherical objects some distance from the Sun. Made in support of Astro204 class at Haverford.

[theodorehalder]

I think the luminosity of the planet's sunny-side equals to the half of the total surface area of the planet. That is, (4πR²)/2 = 2πR². Thanks again.