10 files changed, 242 insertions, 0 deletions
diff --git a/2795/CH3/EX3.1/Ex3_01.sce b/2795/CH3/EX3.1/Ex3_01.sce
new file mode 100755
index 000000000..29351170b
--- /dev/null
+++ b/2795/CH3/EX3.1/Ex3_01.sce
@@ -0,0 +1,14 @@
+// Scilab Code Ex3.1: Page-87 (2013)
+clc; clear
+E = 1.2e+004;    // Electric field, V/m
+B = 8.8e-004;    // Magnetic field, T
+l = 0.05;    // Length of the deflection plates, m
+v0 = E/B;    // Initial velocity of the electron, m/s
+theta = 30;    // Angular deflection of the electron, degrees
+q_ratio_m = E*tand(theta)/(B^2*l);    // Specific charge of the electron, C/kg
+printf("\nThe initial velocity of the electron = %3.1e m/s", v0);
+printf("\nThe specific charge of the electron = %3.1e C/kg", q_ratio_m);
+
+// Result 
+// The initial velocity of the electron = 1.4e+007 m/s
+// The specific charge of the electron = 1.8e+011 C/kg 
+\ No newline at end of file
diff --git a/2795/CH3/EX3.10/Ex3_10.sce b/2795/CH3/EX3.10/Ex3_10.sce
new file mode 100755
index 000000000..3a55d656c
--- /dev/null
+++ b/2795/CH3/EX3.10/Ex3_10.sce
@@ -0,0 +1,19 @@
+// Scilab Code Ex3.10: Page-106 (2013)
+clc; clear
+phi = 2.36;    // Work function of sodium, eV
+N_A = 6.02e+023;    // Avogadro's number
+e = 1.6e-019;    // Energy equivalent of 1 eV, J
+I = 1e-008;    // Intensity of incident radiation, W/Sq.m
+K = 1.00;    // Kinetic energy of the ejected photoelectron, eV
+rho = 0.97;    // Density of Na atoms, g/cc
+M = 23;    // Gram atomic mass of Na, g/mol
+n = N_A*1e+006/M*rho;    // Number of Na atoms per unit volume, atoms/metre-cube
+// Assume a cubic structure, then 1/d^3 = n, solving for d
+d = (1/n)^(1/3);    // Thickness of one layer of sodium atoms, m
+N = n*d;    // Number of exposed atoms per Sq.m
+R = I/(N*e);    // Rate of energy received by each atom, eV/s
+t = (phi+K)/R;    // Time needed to absorb 3.36 eV energy
+printf("\nThe exposure time of light to produce the photoelectron of %4.2f kinetic energy = %4.1f years", K, t/(60*60*24*365.25));
+
+// Result
+// The exposure time of light to produce the photoelectron of 1.00 kinetic energy = 14.7 years 
+\ No newline at end of file
diff --git a/2795/CH3/EX3.11/Ex3_11.sce b/2795/CH3/EX3.11/Ex3_11.sce
new file mode 100755
index 000000000..87f01dc01
--- /dev/null
+++ b/2795/CH3/EX3.11/Ex3_11.sce
@@ -0,0 +1,15 @@
+// Scilab Code Ex3.11: Page-109 (2013)
+clc; clear
+phi = 2.93;    // Work function of lithium, eV
+lambda = 400e-009;    // Wavelength of incident light, m
+e = 1.6e-019;    // Energy equivalent of 1 eV, J
+c = 2.998e+008;    // Speed of light in vacuum, m/s
+h = 6.626e-034;    // Planck's constant, Js
+E = h*c/(lambda*e);    // Energy of incident light, eV
+V0 = E - phi;    // Stopping potential, V
+printf("\nThe energy of incident photons = %4.2f eV", E);
+printf("\nThe stopping potential = %4.2f V", V0);
+
+// Result
+// The energy of incident photons = 3.10 eV
+// The stopping potential = 0.17 V 
+\ No newline at end of file
diff --git a/2795/CH3/EX3.12/Ex3_12.sce b/2795/CH3/EX3.12/Ex3_12.sce
new file mode 100755
index 000000000..e9e955851
--- /dev/null
+++ b/2795/CH3/EX3.12/Ex3_12.sce
@@ -0,0 +1,17 @@
+
+// Scilab Code Ex3.12: Page-109 (2013)
+clc; clear
+phi = 2.93;    // Work function of lithium, eV
+c = 2.998e+008;    // Speed of light in vacuum, m/s
+K = 3.00;    // Kinetic energy of photoelectron, eV
+E = phi + K;    // Total energy of the incident light, eV
+h = 6.626e-034;    // Planck's constant, Js
+e = 1.6e-019;    // Energy equivalent of 1 eV, J
+f = E*e/h;    // Frequency of incident light, Hz
+lambda = c/f;    // Wavelength of the incident light, m
+printf("\nThe frequency of incident light = %4.2e Hz", f);
+printf("\nThe wavelength of the incident light = %4.2f nm", lambda/1e-009);
+
+// Result
+// The frequency of incident light = 1.43e+015 Hz
+// The wavelength of the incident light = 209.37 nm 
diff --git a/2795/CH3/EX3.13/Ex3_13.sce b/2795/CH3/EX3.13/Ex3_13.sce
new file mode 100755
index 000000000..8558f8c86
--- /dev/null
+++ b/2795/CH3/EX3.13/Ex3_13.sce
@@ -0,0 +1,12 @@
+// Scilab Code Ex3.13: Page-110 (2013)
+clc; clear
+lambda = 350;    // Wavelength of incident light, nm
+e = 1.6e-019;    // Energy equivalent of 1 eV, J
+E = 1.250e+003/lambda;    // Total energy of the incident light, eV
+I = 1e-008;    // Intensity of incident light, W/Sq.m
+// As Intensity, I = N*E, solving for N
+N = I/(E*e);    // The number of photons in the light beam
+printf("\nThe number of photons in the light beam = %3.1e photons/Sq.m/s", N);
+
+// Result
+// The number of photons in the light beam = 1.8e+010 photons/Sq.m/s 
+\ No newline at end of file
diff --git a/2795/CH3/EX3.15/Ex3_15.sce b/2795/CH3/EX3.15/Ex3_15.sce
new file mode 100755
index 000000000..6885cf084
--- /dev/null
+++ b/2795/CH3/EX3.15/Ex3_15.sce
@@ -0,0 +1,11 @@
+// Scilab Code Ex3.15: Page-113 (2013)
+clc; clear
+e = 1.6e-019;    // Energy equivalent of 1 eV, J
+c = 2.998e+008;    // Speed of light in vacuum, m/s
+h = 6.626e-034;    // Planck's constant, Js
+V0 = 35e+003;    // Electron acceleration voltage, V
+lambda_min = h*c/(e*V0);    // Duane-Hunt rule for wavelength, m
+printf("\nThe minimum wavelength of X-rays = %4.2e m", lambda_min);
+
+// Result
+// The minimum wavelength of X-rays = 3.55e-011 m 
+\ No newline at end of file
diff --git a/2795/CH3/EX3.16/Ex3_16.sce b/2795/CH3/EX3.16/Ex3_16.sce
new file mode 100755
index 000000000..f9c89c278
--- /dev/null
+++ b/2795/CH3/EX3.16/Ex3_16.sce
@@ -0,0 +1,25 @@
+// Scilab Code Ex3.16: Page-116 (2013)
+clc; clear
+c = 2.998e+008;    // Speed of light in vacuum, m/s
+h = 6.626e-034;    // Planck's constant, Js
+m_e = 9.11e-031;    // Rest mass of an electron, kg
+lambda = 0.050;    // Wavelength of the X-ray, nm
+theta = 180;    // The angle at which the recoil electron Ke becomes the largest, degree
+E_x_ray = 1.240e+003/lambda;    // Energy of the X-ray, eV
+lambda_prime = lambda + (1-cosd(theta))*h/(m_e*c*1e-009);    // The largest wavelength of the scattered photon, nm
+E_prime_x_ray = 1.240e+003/lambda_prime;    // Energy of the scattered photon, eV
+K = (E_x_ray - E_prime_x_ray)/1e+003;    // Kinetic energy of the most energetic recoil electron, keV
+if (E_prime_x_ray < E_x_ray) then
+    printf("\nThe X-ray is Compton-scattered by the electron.");
+else
+    printf("\nThe X-ray is not Compton-scattered by the electron.");
+end
+printf("\nThe largest wavelength of the scattered photon = %5.3f nm", lambda_prime);
+printf("\nThe kinetic energy of the most energetic recoil electron = %3.1f keV", K);
+printf("\nThe angle at which the recoil electron energy is the largest = %d degrees", theta);
+
+// Result
+// The X-ray is Compton-scattered by the electron.
+// The largest wavelength of the scattered photon = 0.055 nm
+// The kinetic energy of the most energetic recoil electron = 2.2 keV
+// The angle at which the recoil electron energy is the largest = 180 degrees 
+\ No newline at end of file
diff --git a/2795/CH3/EX3.3/Ex3_03.sce b/2795/CH3/EX3.3/Ex3_03.sce
new file mode 100755
index 000000000..32c7495c5
--- /dev/null
+++ b/2795/CH3/EX3.3/Ex3_03.sce
@@ -0,0 +1,90 @@
+// Scilab Code Ex3.3: Page-94 (2013)
+clc; clear
+function flag = check_visible(lambda)
+    if lambda >= 400 & lambda < 700 then
+        flag = 1;
+        else flag = 0;
+    end
+endfunction
+R_H = 1.0968e+007;    // Rydberg constanr, per metre
+f = zeros(7);
+// Lyman series
+printf("\nFor Lyman series, the wavelengths are:\n")
+n = 1;    // The lowest level of Lyman series
+for k = 2:1:3
+    lambda = 1/(R_H*(1/n^2-1/k^2))/1e-009;
+    printf("k = %d, %5.1f nm", k, lambda);
+    f(k) = check_visible(lambda); 
+    if f(k) == 1 then
+            printf(" (Visible) \n");
+        else
+            printf(" (Ultraviolet)\n");
+    end
+end
+if f(1)  == 1 | f(2)  == 1 | f(3) == 1 then
+        printf("Some wavelengths of Lyman series fall in the visible region.\n")
+    else
+        printf("All the wavelengths of Lyman series fall in the UV-region.\n")
+    end
+
+// Balmer series
+printf("\nFor Balmer series, the wavelengths are:\n")
+n = 2;    // The lowest level of Balmer series
+for k = 3:1:7
+    lambda = 1/(R_H*(1/n^2-1/k^2))/1e-009;
+    printf("k = %d, %5.1f nm", k, lambda);
+    f(k) = check_visible(lambda);
+        if f(k) == 1 then
+            printf(" (Visible) \n");
+        else
+            printf(" (Ultraviolet)\n");
+    end
+end
+
+// Paschen series
+printf("\nFor Paschen series, the wavelengths are:\n")
+n = 3;    // The lowest level of Lyman series
+for k = 4:1:5
+    lambda = 1/(R_H*(1/n^2-1/k^2))/1e-009;
+    printf("k = %d, %5.1f nm", k, lambda);
+    f(k) = check_visible(lambda); 
+    if f(k) == 1 then
+            printf(" (Visible) \n");
+        else
+            printf(" (Infrared)\n");
+    end
+end
+// For limiting member
+k = %inf;
+lambda = 1/(R_H*(1/n^2-1/k^2))/1e-009;
+printf("k = %d, %5.1f nm", %inf, lambda);
+f(6) = check_visible(lambda);
+if f(6) == 1 then
+            printf(" (Visible) \n");
+        else
+            printf(" (Infrared)\n");
+    end
+if f(4)  == 1 | f(5)  == 1 | f(6) == 1 then
+        printf("Some wavelengths of Paschen series fall in the visible region.")
+    else
+        printf("All the wavelengths of Paschen series fall in the IR-region.")
+    end
+        
+// Result 
+// For Lyman series, the wavelengths are:
+// k = 2, 121.6 nm (Ultraviolet)
+// k = 3, 102.6 nm (Ultraviolet)
+// All the wavelengths of Lyman series fall in the UV-region.
+
+// For Balmer series, the wavelengths are:
+// k = 3, 656.5 nm (Visible) 
+// k = 4, 486.3 nm (Visible) 
+// k = 5, 434.2 nm (Visible) 
+// k = 6, 410.3 nm (Visible) 
+// k = 7, 397.1 nm (Ultraviolet)
+
+// For Paschen series, the wavelengths are:
+// k = 4, 1875.6 nm (Infrared)
+// k = 5, 1282.1 nm (Infrared)
+// k = Inf, 820.6 nm (Infrared)
+// All the wavelengths of Paschen series fall in the IR-region.  
+\ No newline at end of file
diff --git a/2795/CH3/EX3.4/Ex3_04.sce b/2795/CH3/EX3.4/Ex3_04.sce
new file mode 100755
index 000000000..8aae3e4b1
--- /dev/null
+++ b/2795/CH3/EX3.4/Ex3_04.sce
@@ -0,0 +1,11 @@
+// Scilab Code Ex3.4: Page-98 (2013)
+clc; clear
+T = 1600 + 273;    // Temperature of the furnace, K
+b = 2.898e-003;    // Wein's constant, m-K
+lambda_max = ceil(b/(T*1e-009));    // Maximum wavelength from Wein's Displacement Law, nm
+printf("\nThe maximum wavelength emitted from the heated furnace = %4d nm", lambda_max); 
+printf("\nThis wavelength falls in the IR-region.");
+
+// Result
+// The maximum wavelength emitted from the heated furnace = 1548 nm
+// This wavelength falls in the IR-region. 
+\ No newline at end of file
diff --git a/2795/CH3/EX3.5/Ex3_05.sce b/2795/CH3/EX3.5/Ex3_05.sce
new file mode 100755
index 000000000..28bd761f4
--- /dev/null
+++ b/2795/CH3/EX3.5/Ex3_05.sce
@@ -0,0 +1,28 @@
+
+// Scilab Code Ex3.5: Page-98 (2013)
+clc; clear
+lambda_max = 500e-009;    // Maximum intensity wavelength emitted by the sun, m
+b = 2.898e-003;    // Wein's constant, m-K
+sigma = 5.67e-008;    // Stefan's constant, W/Sq.m-K^4
+r = 6.96e+008;    // Radius of the sun, m
+r_E = 6.37e+006;    // Radius of the earth, m
+R_E = 1.49e+011;    // Mean-earth sun distance, m
+S = 4*%pi*r^2;    // Surface area of the sun, Sq.m
+T_sun = b/lambda_max;    // The temperature of the sun's surface, K
+R_T = sigma*T_sun^4;    // Power per unit area radiated by the sun, W/Sq.m
+P_sun = R_T*S;    // The total power radiated from the sun's surface, W
+F = r_E^2/(4*R_E^2);    // Fraction of sun's radiation received by Earth
+P_Earth_received = P_sun*F;    // The radiation received by the Earth from the sun, W
+U_Earth = P_Earth_received*60*60*24;    // The radiation received by the Earth from the sun in one day, J
+R_Earth = P_Earth_received/(%pi*r_E^2);    // Power received by the Earth per unit of exposed area, W/Sq.m
+printf("\nThe surface temperature of the sun = %4d K", ceil(T_sun));
+printf("\nThe power per unit area emitted from the surface of the sun = %4.2e W/Sq.m", R_T);
+printf("\nThe energy received by the Earth each day from the radiation of sun = %4.2e J", U_Earth);
+printf("\nThe power received by the Earth per unit of exposed area = %4d W/Sq.m", ceil(R_Earth));
+
+// Result
+// The surface temperature of the sun = 5796 K
+// The power per unit area emitted from the surface of the sun = 6.40e+007 W/Sq.m
+// The energy received by the Earth each day from the radiation of sun = 1.54e+022 J
+// The power received by the Earth per unit of exposed area = 1397 W/Sq.m 
+// The answers are given wrong in the textbook
+\ No newline at end of file