Homeworks

1. Homeworks Antonio Aguirre EET 3132 Fall 2011 NYCCT/CUNY

2. HW1 • % EET 3132:Remote Sensing, Instr: VivianaVladutescu, Student: Antonio Aguirre • % Sept. 23, 2011 @ New York City College of Technology (CUNY) • % contact: sadykov1@yahoo.com • close all,clear all • %%% Showing a Blackbody radiation plot (lambda vs. blackbody radiation) • % Constants • h=6.626E-34; % Planck's constant (J*s) • c=3E8; % speed of light (m/s) • k=1.38E-23; % Boltzmann's constant (J/K) • sigma=5.67E-8; % Stefan–Boltzmann constant: http://en.wikipedia.org/wiki/Stefan%E2%80%93Boltzmann_constant • lambda=.001e-6:0.01e-6:20e-6; % Lambda in microns • T1=245; % Temperature of Earth in (K) • T2=6000; % Temperature of Sun in (K) • T3=5260; % Temperature of Alpha Centauri B in (K) • % Blackbody radiation equation in 3 parts: for simplicity • A1=(h*c)./(k*T1.*lambda); • A2=(h*c)./(k*T2.*lambda); • A3=(h*c)./(k*T3.*lambda); • B=(2*h*c^2)./lambda.^5; • BB1=B.*(1./(exp(A1)-1)); • BB2=B.*(1./(exp(A2)-1)); • BB3=B.*(1./(exp(A3)-1));

3. % Plot of the radiation curve for the Earth, Sun, and Alpha Centauri B. • subplot(2,1,1) • plot(lambda,BB1,lambda,BB2,lambda,BB3) • % semilogy(lambda,BB1,lambda,BB2,lambda,BB3) • xlabel('Wavelength in microns') • ylabel('Radiance in W*m^-2') • legend('earth bb','sunbb','alpha centaury') • subplot(2,1,2) • plot(lambda,BB1) • % semilogy(lambda,BB1,lambda,BB2,lambda,BB3) • xlabel('Wavelength in microns') • ylabel('Radiance in W*m^-2') • legend('earth bb') • %%% Showing that B(lambda,T)=sigma*T^4 • lambda2=300E-9:10E-9:4000E-9; • Asun=(h*c)./(k*T2.*lambda2); • Bsun=(2*h*c^2)./(lambda2.^5); • BBsun=Bsun.*(1./(exp(Asun)-1)); • display ('B(lambda2,T2)=zz and sigma*T2^4=zz1') • zz=trapz(BBsun) • zz_aBB2=trapz(BB2) • zz1=sigma*(T2^4)

4. HW2 • % EET 3132:Remote Sensing, Instr: VivianaVladutescu, Student: Antonio Aguirre • % Sept. 23, 2011 @ New York City College of Technology (CUNY) • % contact: sadykov1@yahoo.com • clc,clear all • cd('E:\Remote Sensing') % Sets the directory, not necessary. • file='111010_111010_CCNY.lev15'; % Names the file to load • data=importdata(file,','); % Reads the file and seperates data (commas=diff columns) • data_1=data.textdata; % defines the location of the data within the structure • [s,d]=size(data_1); % defines the size in [x,y] dimensions (rows, columns) • for k=6:s % loop for reading from row 6 to the last row. • aod_440(k-5)=str2num(data_1{k,16}); % turning characters to actual numbers from desired column • aod_500(k-5)=str2num(data_1{k,13}); % (k-5) is so that the values are stored starting at 1 and not 6 • aod_675(k-5)=str2num(data_1{k,7}); % {k,n} k is for the row determined by the loop state • aod_870(k-5)=str2num(data_1{k,6}); % {k,n} n is for the column of interest • time(k-5)=str2num(data_1{k,3}); • end

5. time_round=fix(time); % rounding time down to establish whole days • time_fraction=time-time_round; % determining the fraction of the time of day • time_hour=time_fraction*24; % turning it into actual hours • t=time_hour; %UTC • % Vectors for plotting all AOD's vs. time • wav=[440,500,675,870]; • aod=[aod_440(7),aod_500(7),aod_675(7),aod_870(7)]; • % Calculating the Angstrom Exponent • top=log(aod_870/aod_440); • bottom=log(870/440); • angstrom=-(top./bottom) • %plot of AOD vs. Time • subplot(3,1,1) • plot(t,aod_440,'b*-',t,aod_500,'g+-',t,aod_675,'rx-',t,aod_870,'k^-') • legend('AOD 440','AOD 500','AOD 675','AOD 870',0) % the '0' places the legend in the best spot • xlabel('UTC') • ylabel('AOD') • title('AOD vs. Time') • hold on • % Plot AOD vs. Lambda • subplot(3,1,2) • plot(wav,aod,'b*-') • xlabel('Wavelength in (nanometer)') • ylabel('AOD') • title('AOD vs. Wavelength') • legend('AOD',0) • hold on • % Plot Angstrom vs. Time • subplot(3,1,3) • plot(t,angstrom,'m^-') • xlabel('UTC') • ylabel('Angstrom Exponent') • legend('Angstrom Values',0) • title('Angstrom vs. Time')