| Date 06/09/2010 |
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| Script S6_2_3.m | |||
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%==============================================
%planck 3 %Attention! The function fplanck must be used %============================================== % %the Sun temperature in °K T=5800; % %============================================== %the whole Sun intensity using Stefan_Boltzmann law % %the fourth power of the Sun temperature T4=T^4; %Stefan_Boltzmann constant sigma=5.6742e-08; %the whole Sun intensity I_S=sigma*T4 % %============================================== %the whole Sun intensity integrating the Planck law % %interval of N frequencies between numin and numax N=1000000; numin=1000; numax=1.5e015; % %corresponding spectral intensities f=fplanck(T,N,numin,numax); % %whole intensity % I=trapz(f(1,:),f(2,:)) % % %============================================== %the whole Sun intensity in the visible range % %frequencies of the visible interval nuluxmin=4.3e014 nuluxmax=7.4e014 % %corresponding spectral intensitiy in the visible range f1=fplanck(T,N,nuluxmin,nuluxmax); % %whole intensity in the visible range I1=trapz(f1(1,:),f1(2,:)) % %percent value I1perc=(I1*100)/I % %============================================== %The Sun whole and partial power % %Sun radius considered a sphere r=6.960e+008; %area of the Sun sphere surface S_Sun=4*pi*(r^2) %power W_S due to the whole Sun radiation W_S=I_S*S_Sun %the partial Sun power due to the visible radiation W_V=I1*S_Sun % %============================================== %the solar constants % %distance from Sun to Earth R=1.496e+011; %area of the sphere surface S_E (see Problem, pag. 251) S_E=4*pi*(R^2) %whole solar constant Sun_c_w=W_S/S_E %partial solar constant Sun_c_v=W_V/S_E %============================================== % |
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