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Astronomy · L4 · From blackbody temperature to observable stellar properties

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How a blackbody's temperature determines both its emitted flux (Stefan-Boltzmann) and its spectral peak (Wien's law).

by @openstemUpdated Astronomy
Blackbody at temperature TStefan-Boltzmann lawF = σT⁴Wien's displacement lawλ_max = b/TFlux per unit area(steep T⁴ dependence)Total luminosityL = 4πR²σT⁴Peak wavelength / colour(hot = blue, cool = red)Position on theHertzsprung-Russell diagram

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