Black Body Radiation and Wien's Law
Here's where stellar physics gets really clever - we can actually measure a star's temperature just by looking at the colour of light it emits most intensely. Stars behave like black bodies, theoretical objects that absorb and emit all incident radiation.
The black body spectrum shows us that hotter objects emit shorter wavelengths more intensely. As temperature increases, the peak wavelength shifts towards the blue end of the spectrum and becomes much brighter overall.
Wien's displacement law gives us the mathematical relationship: λp = W/T, where W = 2.9 × 10⁻³ m·K. This means peak wavelength is inversely proportional to absolute temperature. Remember to convert Celsius to Kelvin by adding 273.15!
Stefan's law takes this further, stating that power emitted per unit area is proportional to T⁴. For a complete star: P = σAT⁴ = 4πr²σT⁴, where σ = 5.67 × 10⁻⁸ Wm⁻²K⁻⁴.
Pro Tip: The inverse square law explains why distant stars appear dimmer - intensity decreases with the square of distance as radiation spreads over increasingly larger spherical areas.