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Compute blackbody emission spectrum
E = blackbody(lambda, T) is the blackbody radiation power density [W/mˆ3] at the wavelength lambda [m] and temperature T [K].
If lambda is a column vector (Nx1), then E is a column vector (Nx1) of blackbody radiation power density at the corresponding elements of lambda.
l = [380:10:700]'*1e-9; % visible spectrum e = blackbody(l, 6500); % emission of sun plot(l, e)
© 1990-2012 Peter Corke.