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diff --git a/530/CH3/EX3.1/example_3_1.sce b/530/CH3/EX3.1/example_3_1.sce
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+clear;
+clc;
+
+// A Textbook on HEAT TRANSFER by S P SUKHATME
+// Chapter 3
+// Thermal Radiation
+
+// Example 3.1
+// Page 114
+printf("Example 3.1, Page 114 \n\n");
+
+T = 5779 ; // [Temperature,in Kelvin]
+// From Wein's law, eqn 3.2.8
+lambda_m = 0.00290/T ; // [m]
+// Substituting this value in plank's law, we get
+e = 2*(%pi)*0.596*(10^-16)/(((0.5018*10^-6)^5)*(exp(0.014387/0.00290)-1)) ; //[W/m^2 m]
+
+e_bl_max= e / 10^6 ;
+
+printf("Value of emissivity on sun surface is %f W/m^2 um \n",e_bl_max); //[W/m^2 um]
+
+e_earth = e_bl_max*((0.695*10^6)/(1.496*10^8))^2 ;
+
+printf("The value of emmissivity on earths surface is %f W/m^2 um", e_earth)
+\ No newline at end of file