M-File Help: blackbody View code for blackbody

blackbody

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.

Example

l = [380:10:700]'*1e-9; % visible spectrum
e = blackbody(l, 6500); % emission of sun
plot(l, e)

References


 

© 1990-2012 Peter Corke.