Blackbody curves

According to Planck's law of blackbody radiation, spectral energy density of radiation emitted from a blackbody in \(W \over m^3\) as a function of wavelength \( \lambda \) at a temperature \(T\) in Kelvin is given by the equation: $$ R = {{2 h c^2} \over \lambda^5}{1\over {e^{{hc}\diagup{k_B \lambda T}}}-1} $$ Where \(h\) is Planck's constant \(6.63 \times 10^-23\) \({Joule*second}\), \(c\) is the speed of light \({3 \times 10^8} {meter \over second}\), and \(k_B\) is Boltzmann's constant \(1.39 \times 10^{-23} {Joule \over Kelvin}\)

Wien's displacement law allows for calculating the peak of the radiation curve which shifts with the temperature as described in Planck's law of blackbody radiation. The peak wavelength \( \lambda_{peak}\) of the blackbody emission curve can be calculated by the following equation. $$\lambda{peak} = {{hc} \over x}{1 \over {k_B \lambda T}} $$ In this equation \(x\) is a constant parameter equal to \(4.965114231744276\).

Note: Blackbody radiation relies on an idealized concept. In application, radiation curves may experience wavelength dependence based on material characteristics.

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