initial commit / add all books

11 files changed, 328 insertions, 0 deletions

diff --git a/534/CH12/EX12.1/12_1_Plate_surface.sce b/534/CH12/EX12.1/12_1_Plate_surface.sce
new file mode 100644
index 000000000..953567f5f
--- /dev/null
+++ b/534/CH12/EX12.1/12_1_Plate_surface.sce
@@ -0,0 +1,34 @@
+clear;

+clc;

+printf('FUNDAMENTALS OF HEAT AND MASS TRANSFER \n Incropera / Dewitt / Bergman / Lavine \n EXAMPLE 12.1   Page 731 \n')// Example 12.1

+

+// a) Intensity of emission in each of the three directions

+// b) Solid angles subtended by the three surfaces

+// c) Rate at which radiation is intercepted by the three surfaces

+

+A1 = .001		;//[m^2] Area of emitter

+In  = 7000		;//[W/m^2.Sr] Intensity of radiation in normal direction

+A2 = .001		;//[m^2] Area of other intercepting plates

+A3 = A2			;//[m^2] Area of other intercepting plates

+A4 = A2			;//[m^2] Area of other intercepting plates

+r = .5			;//[m] Distance of each plate from emitter

+theta1 = 60		;//[deg] Angle between surface 1 normal & direction of radiation to surface 2

+theta2 = 30		;//[deg] Angle between surface 2 normal & direction of radiation to surface 1

+theta3 = 45		;//[deg] Angle between surface 1 normal & direction of radiation to surface 4

+

+//From equation 12.2

+w31 = A3/r^2;

+w41 = w31;

+w21 = A2*cos(theta2*0.0174532925)/r^2;

+

+

+//From equation 12.6

+q12 = In*A1*cos(theta1*0.0174532925)*w21;

+q13 = In*A1*cos(0)*w31;

+q14 = In*A1*cos(theta3*0.0174532925)*w41;

+

+printf("\n (a) As Intensity of emitted radiation is independent of direction, for each of the three directions I = %i W/m^2.sr \n\n (b) By the Three Surfaces\n         Solid angles subtended                Rate at which radiation is intercepted \n           w4-1 = %.2e sr                           q1-4 = %.1e W \n           w3-1 = %.2e sr                           q1-3 = %.1e W\n           w2-1 = %.2e sr                           q1-2 = %.1e W    ",In,w41,q14,w31,q13,w21,q12);

+//END

+

+

+

diff --git a/534/CH12/EX12.10/12_10_Metallic_Sphere.sce b/534/CH12/EX12.10/12_10_Metallic_Sphere.sce
new file mode 100644
index 000000000..101f8e4a5
--- /dev/null
+++ b/534/CH12/EX12.10/12_10_Metallic_Sphere.sce
@@ -0,0 +1,26 @@
+clear;

+clc;

+printf('FUNDAMENTALS OF HEAT AND MASS TRANSFER \n Incropera / Dewitt / Bergman / Lavine \n EXAMPLE 12.10   Page 768 \n')// Example 12.10

+

+// Total hemispherical absorptivity and emissivity of sphere for initial condition

+// values of absoprtivity and emissivity after sphere has been in furnace a long time

+

+Ts = 300;			//[K] temperature of surface

+Tf = 1200;           //[K] Temperature of Furnace

+stfncnstt = 5.67*10^-8;		//[W/m^2.K^4] Stefan-Boltzmann constant

+// From the given graph of absorptivities

+a1 = .8;    //between wavelength 0 micro-m- 5 micro-m

+a2 = .1;    //greater than wavelength 5 micro-m

+

+//From Table 12.1

+//For wl1 = 5 micro-m and T = 1200 K, At wl1*T = 6000 micro-m.K

+F0wl1 = 0.738;

+//From equation 12.44

+a = a1*F0wl1 + a2*(1-F0wl1);

+//From Table 12.1

+//For wl1 = 5 micro-m and T = 300 K, At wl1*T = 1500 micro-m.K

+F0wl1s = 0.014;

+//From equation 12.36

+e = a1*F0wl1s + a2*(1-F0wl1s);

+

+printf('\n For Initial Condition \n Total hemispherical absorptivity = %.2f     Emissivity of sphere = %.2f \n\n Beacuase the spectral characteristics of the coating and the furnace temeprature remain fixed, there is no change in the value of absorptivity with increasing time. \n Hence, After a sufficiently long time, Ts = Tf = %i K and emissivity equals absorptivity e = a = %.2f',a,e,Tf,a);
\ No newline at end of file
diff --git a/534/CH12/EX12.11/12_11_Solar_Collector.sce b/534/CH12/EX12.11/12_11_Solar_Collector.sce
new file mode 100644
index 000000000..645ac0b7b
--- /dev/null
+++ b/534/CH12/EX12.11/12_11_Solar_Collector.sce
@@ -0,0 +1,28 @@
+clear;

+clc;

+printf('FUNDAMENTALS OF HEAT AND MASS TRANSFER \n Incropera / Dewitt / Bergman / Lavine \n EXAMPLE 12.11   Page 774 \n')// Example 12.11

+

+// Useful heat removal rate per unit area

+// Efficiency of the collector

+

+Ts = 120+273;			//[K] temperature of surface

+Gs = 750;                 //[W/m^2] Solar irradiation

+Tsky = -10+273;          //[K] Temperature of Sky

+Tsurr = 30+273;          //[K] Temperature os surrounding Air

+e = .1                  ;// emissivity 

+as = .95                ;// Absorptivity of Surface

+asky = e                ;// Absorptivity of Sky

+stfncnstt = 5.67*10^-8;		//[W/m^2.K^4] Stefan-Boltzmann constant

+h = 0.22*(Ts - Tsurr)^.3334    ;//[W/m^2.K] Convective Heat transfer Coeff

+//From equation 12.67

+Gsky = stfncnstt*Tsky^4;      //[W/m^2]  Irradiadtion from sky

+qconv = h*(Ts-Tsurr);        //[W/m^2]  Convective Heat transfer

+E = e*stfncnstt*Ts^4;       //[W/m^2]  Irradiadtion from Surface

+

+//From energy Balance

+q = as*Gs + asky*Gsky - qconv - E;

+

+//Collector efficiency

+eff = q/Gs;

+

+printf('\n Useful heat removal rate per unit area by Energy Conservation = %i W/m^2 \n Collector efficiency defined as the fraction of solar irradiation extracted as useful energy is %.2f',q,eff);
\ No newline at end of file
diff --git a/534/CH12/EX12.2/12_2_Spectral_Distribution.sce b/534/CH12/EX12.2/12_2_Spectral_Distribution.sce
new file mode 100644
index 000000000..c39690689
--- /dev/null
+++ b/534/CH12/EX12.2/12_2_Spectral_Distribution.sce
@@ -0,0 +1,19 @@
+clear;

+clc;

+printf('FUNDAMENTALS OF HEAT AND MASS TRANSFER \n Incropera / Dewitt / Bergman / Lavine \n EXAMPLE 12.2   Page 734\n')// Example 12.2

+

+// Total Irradiation

+x=[0 5 20 25];

+y=[0 1000 1000 0];

+clf();

+plot2d(x,y,style=5,rect=[0,0,30,1100]);

+xtitle("Spectral Distribution", "wavelength (micro-m)", "G (W/m^2.micro-m)");

+

+//By Equation 12.4

+G = 1000*(5-0)/2+1000*(20-5)+1000*(25-20)/2;

+

+printf("\n G = %i W/m^2",G);

+//END

+

+

+

diff --git a/534/CH12/EX12.3/12_3_Blackbody_Radiation.sce b/534/CH12/EX12.3/12_3_Blackbody_Radiation.sce
new file mode 100644
index 000000000..7c8c97943
--- /dev/null
+++ b/534/CH12/EX12.3/12_3_Blackbody_Radiation.sce
@@ -0,0 +1,34 @@
+clear;

+clc;

+printf('FUNDAMENTALS OF HEAT AND MASS TRANSFER \n Incropera / Dewitt / Bergman / Lavine \n EXAMPLE 12.3   Page 741 \n')// Example 12.3

+

+// Spectral Emissive Power of a small aperture on the enclosure

+// wavelengths below which and above which 10% of the radiation is concentrated

+// Spectral emissive power and wavelength associated with maximum emission

+// Irradiation on a small object inside the enclosure

+

+T = 2000			;//[K] temperature of surface

+stfncnstt = 5.67*10^-8		;//[W/m^2.K^4] Stefan-Boltzmann constant

+E = stfncnstt*T^4;        //[W/m^2]

+

+//From Table 12.1 

+constt1 = 2195    ;    //[micro-m.K]

+wl1 = constt1/T;

+//From Table 12.1 

+constt2 = 9382   ;     //[micro-m.K]

+wl2 = constt2/T;

+

+//From Weins Law, wlmax*T = consttmax = 2898 micro-m.K

+consttmax = 2898         ;//micro-m.K

+wlmax = consttmax/T;

+//from Table 12.1 at wlmax = 1.45 micro-m.K and T = 2000 K

+I = .722*10^-4*stfncnstt*T^5;

+Eb = %pi*I;

+

+G = E;        //[W/m^2] Irradiation of any small object inside the enclosure is equal to emission from blackbody at enclosure temperature

+

+printf("\n (a) Spectral Emissive Power of a small aperture on the enclosure = %.2e W/m^2.Sr for each of the three directions \n (b) Wavelength below which 10percent of the radiation is concentrated = %.1f micro-m \n     Wavelength above which 10percent of the radiation is concentrated = %.2f micro-m \n (c) Spectral emissive power and wavelength associated with maximum emission is %.2e micro-m and %.2e W/m^2.micro-m respectively \n (d) Irradiation on a small object inside the enclosure = %.2e W/m^2",E,wl1,wl2,Eb,wlmax,G);

+//END

+

+

+

diff --git a/534/CH12/EX12.4/12_4_Blackbody_Angular_Radiation.sce b/534/CH12/EX12.4/12_4_Blackbody_Angular_Radiation.sce
new file mode 100644
index 000000000..6015f17bc
--- /dev/null
+++ b/534/CH12/EX12.4/12_4_Blackbody_Angular_Radiation.sce
@@ -0,0 +1,26 @@
+clear;

+clc;

+printf('FUNDAMENTALS OF HEAT AND MASS TRANSFER \n Incropera / Dewitt / Bergman / Lavine \n EXAMPLE 12.4   Page 743 \n')// Example 12.4

+

+// Rate of emission per unit area over all directions between 0 degC and 60 degC and over all wavelengths between wavelengths 2 and 4 micro-m

+

+T = 1500			;//[K] temperature of surface

+stfncnstt = 5.67*10^-8		;//[W/m^2.K^4] Stefan-Boltzmann constant

+

+//From Equation 12.26 Black Body Radiation

+Eb = stfncnstt*T^4;        //[W/m^2]

+

+//From Table 12.1 as wl1*T = 2*1500 (micro-m.K)

+F02 = .273;

+//From Table 12.1 as wl2*T = 4*1500 (micro-m.K)

+F04 = .738;

+

+//From equation 12.10 and 12.11

+i1 = integrate('2*cos(x)*sin(x)','x',0,%pi/3);

+delE = i1*(F04-F02)*Eb;

+

+printf("\n Rate of emission per unit area over all directions between 0 degC and 60 degC and over all wavelengths between wavelengths 2 micro-m and 4 micro-m = %.1e W/m^2",delE);

+//END

+

+

+

diff --git a/534/CH12/EX12.5/12_5_Diffuse_emitter.sce b/534/CH12/EX12.5/12_5_Diffuse_emitter.sce
new file mode 100644
index 000000000..8d2f40319
--- /dev/null
+++ b/534/CH12/EX12.5/12_5_Diffuse_emitter.sce
@@ -0,0 +1,45 @@
+clear;

+clc;

+printf('FUNDAMENTALS OF HEAT AND MASS TRANSFER \n Incropera / Dewitt / Bergman / Lavine \n EXAMPLE 12.5   Page 748 \n')// Example 12.5

+

+// Total hemispherical emissivity

+// Total emissive Power

+// Wavelength at which spectral emissive power will be maximum

+

+T = 1600			;//[K] temperature of surface

+wl1 = 2            ;//[micro-m] wavelength 1

+wl2 = 5            ;//[micro-m] wavelength 2

+stfncnstt = 5.67*10^-8;		//[W/m^2.K^4] Stefan-Boltzmann constant

+// From the given graph of emissivities

+e1 = .4;

+e2 = .8;

+//From Equation 12.26 Black Body Radiation

+Eb = stfncnstt*T^4;        //[W/m^2]

+

+//Solution (A)

+//From Table 12.1 as wl1*T = 2*1600 (micro-m.K)

+F02 = .318;

+//From Table 12.1 as wl2*T = 5*1600 (micro-m.K)

+F05 = .856;

+//From Equation 12.36

+e = e1*F02 + e2*[F05 - F02];

+

+//Solution (B)

+//From equation 12.35

+E = e*Eb;

+

+//Solution (C)

+//For maximum condition Using Weins Law

+consttmax = 2898        ;//[micro-m.K]

+wlmax = consttmax/T;

+

+//equation 12.32 with Table 12.1

+E1 = %pi*e1*.722*10^-4*stfncnstt*T^5;

+

+E2 = %pi*e2*.706*10^-4*stfncnstt*T^5;

+

+printf("\n (a) Total hemispherical emissivity = %.3f \n (b) Total emissive Power = %i kW/m^2 \n (c) Emissive Power at wavelength 2micro-m is greater than Emissive power at maximum wavelength \n     i.e. %.1f kW/m^2 > %.1f kW/m^2 \n     Thus, Peak emission occurs at %i micro-m",e,E/1000,E2/1000,E1/1000,wl1);

+//END

+

+

+

diff --git a/534/CH12/EX12.6/12_6_Metallic_surface.sce b/534/CH12/EX12.6/12_6_Metallic_surface.sce
new file mode 100644
index 000000000..2a4c4b7f7
--- /dev/null
+++ b/534/CH12/EX12.6/12_6_Metallic_surface.sce
@@ -0,0 +1,32 @@
+clear;

+clc;

+printf('FUNDAMENTALS OF HEAT AND MASS TRANSFER \n Incropera / Dewitt / Bergman / Lavine \n EXAMPLE 12.6   Page 751 \n')// Example 12.6

+

+// Spectral , Normal emissivity en and spectral hemispherical emissivity e

+// Spectral normal intensity In and Spectral emissive power

+

+T = 2000			;//[K] temperature of surface

+wl = 1            ;//[micro-m] wavelength 

+stfncnstt = 5.67*10^-8;		//[W/m^2.K^4] Stefan-Boltzmann constant

+

+// From the given graph of emissivities

+e1 = .3;

+e2 = .6;

+//From Equation 12.26 Black Body Radiation

+Eb = stfncnstt*T^4;        //[W/m^2]

+

+//Equation 12.34

+i1 = integrate('e1*cos(x)*sin(x)','x',0,%pi/3);

+i2 = integrate('e2*cos(x)*sin(x)','x',%pi/3,4*%pi/9);

+e = 2*[i1+i2];

+

+// From Table 12.1 at wl = 1 micro-m and T = 2000 K.

+

+I = .493*10^-4 * stfncnstt*T^5        ;//[W/m^2.micro-m.sr]

+

+In = e1*I;

+

+//Using Equation 12.32 for wl = 1 micro-m and T = 2000 K

+E = e*%pi*I;

+

+printf('\n Spectral Normal emissivity en = %.1f and spectral hemispherical emissivity e = %.2f \n Spectral normal intensity In = %.2e W/m^2.micro-m.sr and Spectral emissive power = %.1e W/m^2.micro-m.sr ', e1, e,In,E);
\ No newline at end of file
diff --git a/534/CH12/EX12.7/12_7_Opaque_surface.sce b/534/CH12/EX12.7/12_7_Opaque_surface.sce
new file mode 100644
index 000000000..941a2e172
--- /dev/null
+++ b/534/CH12/EX12.7/12_7_Opaque_surface.sce
@@ -0,0 +1,29 @@
+clear;

+clc;

+printf('FUNDAMENTALS OF HEAT AND MASS TRANSFER \n Incropera / Dewitt / Bergman / Lavine \n EXAMPLE 12.7   Page 759 \n')// Example 12.7

+

+// Spectral distribution of reflectivity

+// Total, hemispherical absorptivity

+// Nature of surface temperature change

+

+T = 500			;//[K] temperature of surface

+e = .8;

+stfncnstt = 5.67*10^-8;		//[W/m^2.K^4] Stefan-Boltzmann constant

+

+x=[0 6 8 16];

+y=[.8 .8 0 0];

+clf();

+plot2d(x,y,style=5,rect=[0,0,20,1]);

+

+

+xtitle("Spectral Distribution of reflectivity", "wavelength (micro-m)", "reflectivity");

+

+//From equation 12.43 and 12.44

+Gabs = {.2*500/2*(6-2)+500*[.2*(8-6)+(1-.2)*(8-6)/2]+1*500*(12-8)+500*(16-12)/2}            ;//[w/m^2]

+G = {500*(6-2)/2+500*(12-6)+500*(16-12)/2}            ;//[w/m^2]

+a = Gabs/G;

+

+//Neglecting convection effects net het flux to the surface

+qnet = a*G - e*stfncnstt*T^4;

+

+printf('\n Total, hemispherical absorptivity %.2f \n Nature of surface temperature change = %i W/m^2 \n Since qnet > 0, the sirface temperature will increase with the time', a,qnet);
\ No newline at end of file
diff --git a/534/CH12/EX12.8/12_8_Glass_Cover.sce b/534/CH12/EX12.8/12_8_Glass_Cover.sce
new file mode 100644
index 000000000..c723347b9
--- /dev/null
+++ b/534/CH12/EX12.8/12_8_Glass_Cover.sce
@@ -0,0 +1,20 @@
+clear;

+clc;

+printf('FUNDAMENTALS OF HEAT AND MASS TRANSFER \n Incropera / Dewitt / Bergman / Lavine \n EXAMPLE 12.8   Page 761 \n')// Example 12.8

+

+// Total emissivity of cover glass to solar radiation

+

+T = 5800			;//[K] temperature of surface

+e = .8;

+stfncnstt = 5.67*10^-8;		//[W/m^2.K^4] Stefan-Boltzmann constant

+

+//From Table 12.1

+//For wl1 = .3 micro-m and T = 5800 K, At wl1*T = 1740 micro-m.K

+F0wl1 = .0335;

+//For wl1 = .3 micro-m and T = 5800 K, At wl2*T = 14500 micro-m.K

+F0wl2 = .9664;

+

+//Hence from equation 12.29

+t = .90*[F0wl2 - F0wl1];

+

+printf('\n Total emissivity of cover glass to solar radiation = %.2f',t);
\ No newline at end of file
diff --git a/534/CH12/EX12.9/12_9_Brick_Wall.sce b/534/CH12/EX12.9/12_9_Brick_Wall.sce
new file mode 100644
index 000000000..55c598a70
--- /dev/null
+++ b/534/CH12/EX12.9/12_9_Brick_Wall.sce
@@ -0,0 +1,35 @@
+clear;

+clc;

+printf('FUNDAMENTALS OF HEAT AND MASS TRANSFER \n Incropera / Dewitt / Bergman / Lavine \n EXAMPLE 12.9   Page 766 \n')// Example 12.9

+

+// Total hemispherical emissivity of fire brick wall

+// Total emissive power of brick wall

+// Absorptivity of the wall to irradiation from coals

+

+Ts = 500			;//[K] temperature of brick surface

+Tc = 2000           ;//[K] Temperature of coal exposed

+stfncnstt = 5.67*10^-8;		//[W/m^2.K^4] Stefan-Boltzmann constant

+// From the given graph of emissivities

+e1 = .1;    //between wavelength 0 micro-m- 1.5 micro-m

+e2 = .5;    //between wavelength 1.5 micro-m- 10 micro-m

+e3 = .8;    //greater than wavelength 10 micro-m

+

+//From Table 12.1

+//For wl1 = 1.5 micro-m and T = 500 K, At wl1*T = 750 micro-m.K

+F0wl1 = 0;

+//For wl2 = 10 micro-m and T = 500 K, At wl2*T = 5000 micro-m.K

+F0wl2 = .634;

+//From equation 12.36

+e = e1*F0wl1 + e2*F0wl2 + e3*(1-F0wl1-F0wl2);

+

+//Equation 12.26 and 12.35

+E = e*stfncnstt*Ts^4;

+

+//From Table 12.1

+//For wl1 = 1.5 micro-m and T = 2000 K, At wl1*T = 3000 micro-m.K

+F0wl1c = 0.273;

+//For wl2 = 10 micro-m and T = 2000 K, At wl2*T = 20000 micro-m.K

+F0wl2c = .986;

+ac = e1*F0wl1c + e2*[F0wl2c-F0wl1c] + e3*(1-F0wl2c);

+

+printf('\n Total hemispherical emissivity of fire brick wall = %.3f \n Total emissive power of brick wall = %i W/m^2.\n Absorptivity of the wall to irradiation from coals = %.3f',e,E,ac);
\ No newline at end of file