diff options
Diffstat (limited to '2780/CH3')
37 files changed, 362 insertions, 0 deletions
diff --git a/2780/CH3/EX3.1/Ex3_1.sce b/2780/CH3/EX3.1/Ex3_1.sce new file mode 100755 index 000000000..6a742a9e7 --- /dev/null +++ b/2780/CH3/EX3.1/Ex3_1.sce @@ -0,0 +1,16 @@ +clc
+//to calculate angular width and linear width
+lambda=6*10^-5
+e=0.01 //width of slit in cm
+//position of minima is given by
+sintheta=lambda/e //sintheta=m*lambda/e ,where m=1,2,3,......
+disp("sintheta="+string(sintheta)+" m")
+//since theta is very small,so sintheta is approximately equal to theta
+theta=sintheta
+theta1=2*theta
+disp("total angular width of central maximum is theta1="+string(theta1)+" m radians ")
+d=100 //distance in cm
+Y=theta*d
+Y1=2*Y
+disp("linear width of central maximum on the screen is Y1="+string(Y1)+" m cm")
+disp("values of m =1,2,3,............ gives the directions of first, second .............minima")
diff --git a/2780/CH3/EX3.10/Ex3_10.sce b/2780/CH3/EX3.10/Ex3_10.sce new file mode 100755 index 000000000..564b679d5 --- /dev/null +++ b/2780/CH3/EX3.10/Ex3_10.sce @@ -0,0 +1,13 @@ +clc
+//to calculate wavelength of light and missing orders
+omega=0.25 //fringe width in cm
+D=170 //distance in cm
+twod=0.04 // distance in cm
+lambda=omega*twod/D
+disp("wavelength of light is lambda="+string(lambda)+"cm")
+e=0.08 //width of slit in mm
+d=0.4 //in mm
+m=1
+n=m*(e+d)/e
+disp("missing order is n="+string(n)+"unitless")
+//we can also find order for m=2,3,....
diff --git a/2780/CH3/EX3.11/Ex3_11.sce b/2780/CH3/EX3.11/Ex3_11.sce new file mode 100755 index 000000000..42527cc8c --- /dev/null +++ b/2780/CH3/EX3.11/Ex3_11.sce @@ -0,0 +1,7 @@ +clc
+//to calculate wavelength
+n=2 //order of spectrum
+theta=%pi/6 //in radians
+E=1/5000 //let (e+d)=E
+lambda=E*sin(%pi/6)/n
+disp("the wavelength of the spectral line is lambda="+string(lambda)+"cm")
diff --git a/2780/CH3/EX3.12/Ex3_12.sce b/2780/CH3/EX3.12/Ex3_12.sce new file mode 100755 index 000000000..6d1d24660 --- /dev/null +++ b/2780/CH3/EX3.12/Ex3_12.sce @@ -0,0 +1,9 @@ +clc
+//to calculate difference in deviations
+lambda=5*10^-5 //wavelength of light in cm
+eplusd=1/6000 //where eplusd=e+d
+theta1=asind(lambda/eplusd) //for first order spectrum
+theta3=asind(3*lambda/eplusd) //for second order spectrum
+difference=theta3-theta1
+disp("difference in deviations in first and third order spectra is difference ="+string(difference)+"degree")
+
diff --git a/2780/CH3/EX3.13/Ex3_13.sce b/2780/CH3/EX3.13/Ex3_13.sce new file mode 100755 index 000000000..8a243b545 --- /dev/null +++ b/2780/CH3/EX3.13/Ex3_13.sce @@ -0,0 +1,10 @@ +clc
+//to calculate orders
+//let E=(e+d)
+//formula is (e+d)*sin thita=n*lambda
+//for maximum order to be possible thita=90 degree
+//sin theta=1
+E=2.54/2620 //in cm
+lambda=5*10^-5 //wavelength of the incident light in cm
+n=E/lambda
+disp("the orders will be visible is n="+string(n)+"unitless")
diff --git a/2780/CH3/EX3.14/Ex3_14.sce b/2780/CH3/EX3.14/Ex3_14.sce new file mode 100755 index 000000000..e974aa3a5 --- /dev/null +++ b/2780/CH3/EX3.14/Ex3_14.sce @@ -0,0 +1,15 @@ +clc
+//to calculate number of lines in the grating
+//theta1=theta2=30 degree
+//sin theta1=sin theta2=1/2
+lambda1=6*10^-5
+ //wavelength in cm
+lambda2=4.5*10^-5
+//let (e+d)=E
+//formula is (e+d)*sin theta1=n*lambda1----------eq(1)
+//(e+d)*sin theta2=(n+1)*lambda2----------eq(2)
+//we get,
+n=lambda2/(lambda1-lambda2) //order of spectrum
+E=n*lambda1/sin(%pi/6)
+number=1/E
+disp("number of lines is number="+string(number)+"unitless")
diff --git a/2780/CH3/EX3.15/Ex3_15.sce b/2780/CH3/EX3.15/Ex3_15.sce new file mode 100755 index 000000000..457c2fcbc --- /dev/null +++ b/2780/CH3/EX3.15/Ex3_15.sce @@ -0,0 +1,11 @@ +clc
+//to calculate order when visible light of wavelength in the range 4000 to 7500 angstrom
+//let E=(e+d)
+E=1/4000 //in cm
+lambda1=4*10^-5
+ //wavelength in cm
+lambda2=7.5*10^-5
+n1=E*sin(%pi/2)/lambda1
+n2=E*sin(%pi/2)/lambda2
+disp("order when wavelength of 4000 angstrom is n1="+string(n1)+"unitless")
+disp("order when wavelength of 7500 angstrom is n2="+string(n2)+"unitless")
diff --git a/2780/CH3/EX3.17/Ex3_17.sce b/2780/CH3/EX3.17/Ex3_17.sce new file mode 100755 index 000000000..43f1b6dd2 --- /dev/null +++ b/2780/CH3/EX3.17/Ex3_17.sce @@ -0,0 +1,7 @@ +clc
+//to calculate angle of diffraction
+n=1 //order
+lambda=5000*10^-8 //wavelength of light in cm
+eplusd=1/5000 // in cm
+theta=asind(n*lambda/(eplusd))
+disp("angle of diffraction for maximum intensity in the first order is theta="+string(theta)+"degree")
diff --git a/2780/CH3/EX3.18/Ex3_18.sce b/2780/CH3/EX3.18/Ex3_18.sce new file mode 100755 index 000000000..0915750f3 --- /dev/null +++ b/2780/CH3/EX3.18/Ex3_18.sce @@ -0,0 +1,10 @@ +clc
+//to calculate number of lines in one centimeter of the grating
+//let E=(e+d)
+//formula for grating equation for principal maxima is (e+d)*sin theta=n*lambda
+n=2 //order of spectrum
+lambda=5*10^-5 //wavelength in cm
+E=n*lambda/sin(%pi/6)
+number=1/E
+disp("number of lines is number="+string(number)+"unitless")
+//answer is given wrong in the book ,number of lines=1000
diff --git a/2780/CH3/EX3.19/Ex3_19.sce b/2780/CH3/EX3.19/Ex3_19.sce new file mode 100755 index 000000000..9844e9764 --- /dev/null +++ b/2780/CH3/EX3.19/Ex3_19.sce @@ -0,0 +1,12 @@ +clc
+//to calculate which spectral line in 5th order will overlap with 4th order line of 5890 angstrom
+//the grating equation for principal maxima is (e+d)*sin theta =n*lambda
+n1=5
+ //order of spectrum
+n2=4
+lambda2=5890*10^-8 //wavelength of 4th order spectrum in cm
+//(e+d)*sin theta=5*lambda-------------eq(1)
+//(e+d)*sin theta=4*5890*10^-8-----------------eq(2)
+//from eq(1) and eq(2) ,we get
+lambda1=n2*lambda2/n1
+disp("wavelength of 5th order spectrum is lambda1="+string(lambda1)+"cm")
diff --git a/2780/CH3/EX3.2/Ex3_2.sce b/2780/CH3/EX3.2/Ex3_2.sce new file mode 100755 index 000000000..4dc0683d4 --- /dev/null +++ b/2780/CH3/EX3.2/Ex3_2.sce @@ -0,0 +1,11 @@ +clc
+//to calculate wavelength of light
+//in a diffraction pattern due to single slit, minima is given by e*sintheta=m*lambda
+//since theta is very small, sintheta is approximately equal to theta
+//theta=Y/d
+e=0.014 //width of slit in cm
+d=200 //distance in cm
+m=2
+Y=1.6 //in cm
+lambda=Y*e/(d*m)
+disp("wavelength of light is lambda="+string(lambda)+"cm")
diff --git a/2780/CH3/EX3.20/Ex3_20.sce b/2780/CH3/EX3.20/Ex3_20.sce new file mode 100755 index 000000000..d5aa37d94 --- /dev/null +++ b/2780/CH3/EX3.20/Ex3_20.sce @@ -0,0 +1,12 @@ +clc
+//to calculate grating element
+//grating equation for principal maxima is given by (e+d)*sintheta=n*lambda
+//let nth order spectrum for yellow line (lambda=6000 angstrom) coincide with (n+1)th order spectrum for blue line (lambda=4800 angstrom)
+//(e+d)*sintheta=n*6000*10^-8..eq(1)
+//(e+d)*sintheta=(n+1)*4800*10^-8.....eq(2)
+//from eq(1) and eq(2),we get n=4
+n=4
+lambda=6000*10^-8 //wavelength in cm
+sintheta=3/4
+eplusd=n*lambda/sintheta
+disp("grating element is eplusd="+string(eplusd)+"cm")
diff --git a/2780/CH3/EX3.21/Ex3_21.sce b/2780/CH3/EX3.21/Ex3_21.sce new file mode 100755 index 000000000..758dfd3e6 --- /dev/null +++ b/2780/CH3/EX3.21/Ex3_21.sce @@ -0,0 +1,13 @@ +clc
+//to calculate angle of diffraction for third order spectrum and absent spectra if any
+n=3
+lambda=6000*10^-8
+eplusd=1/200
+theta=asind(n*lambda/eplusd)
+disp("angle of refraction is theta="+string(theta)+"degree")
+d=0.0025
+e=eplusd-d //width of wire in cm
+m=1
+n=eplusd*m/e
+disp("order of absent spectrum is n="+string(n)+"unitless")
+disp("here,m=1 is considered because the higher values of m result the order of absent spectrum more than the given order 3")
diff --git a/2780/CH3/EX3.22/Ex3_22.sce b/2780/CH3/EX3.22/Ex3_22.sce new file mode 100755 index 000000000..1b56e2b62 --- /dev/null +++ b/2780/CH3/EX3.22/Ex3_22.sce @@ -0,0 +1,10 @@ +clc
+//to calculate difference in the two wavelengths
+//grating equation for principal maxima is (e+d)*sintheta=n*lambda...............eq(1)
+//differentiate both sides ,we get dtheta=n*dlambda/((e+d)*costheta)...........eq(2)
+lambda=5000 //mean value of wavelengths in angstrom
+cottheta=1.732 //cot30degree=1.732
+dtheta=0.01 //in radian
+//put the value of n from eq(2),we can write eq(2)
+dlambda=lambda*dtheta*cottheta
+disp("difference in two wavelengths is dlambda="+string(dlambda)+"angstrom")
diff --git a/2780/CH3/EX3.23/Ex3_23.sce b/2780/CH3/EX3.23/Ex3_23.sce new file mode 100755 index 000000000..9100eabea --- /dev/null +++ b/2780/CH3/EX3.23/Ex3_23.sce @@ -0,0 +1,10 @@ +clc
+//to calculate dispersive power
+//differentiate grating equation ,we get dtheta/dlambda=n/((e+d)*costheta)
+n=2 //order
+eplusd=1/4000
+lambda=5000*10^-8 //wavelength in cm
+sintheta=n*lambda/(eplusd)
+costheta=sqrt(1-(sintheta)^2)
+dtheta=n/((eplusd)*costheta) //where dispersive power dtheta/dlambda=dtheta
+disp("dispersive power of he grating in the second order spectrum is dtheta="+string(dtheta)+"unitless")
diff --git a/2780/CH3/EX3.24/Ex3_24.sce b/2780/CH3/EX3.24/Ex3_24.sce new file mode 100755 index 000000000..9b8226759 --- /dev/null +++ b/2780/CH3/EX3.24/Ex3_24.sce @@ -0,0 +1,10 @@ +clc
+//to calculate orders
+eplusd=1/4000
+lambda1=5*10^-5
+ //wavelengh in cm
+lambda2=7.5*10^-5
+nmax1=eplusd/lambda1
+nmax2=eplusd/lambda2
+disp("orders will be observed by a grating ,if it is illuminated by light of wavelength of 5000 angstrom is nmax1="+string(nmax1)+"unitless ")
+disp("orders will be observed ,if it is illuminated by light of wavelength of 7500 angstrom is nmax2='+string(nmax2)+"unitless")
diff --git a/2780/CH3/EX3.25/Ex3_25.sce b/2780/CH3/EX3.25/Ex3_25.sce new file mode 100755 index 000000000..2aaf66163 --- /dev/null +++ b/2780/CH3/EX3.25/Ex3_25.sce @@ -0,0 +1,11 @@ +clc
+//to calculate difference in wavelengths of two lines
+//let E=(e+d)=1/5000
+//we get
+E=2*10^-4 //in cm
+n=2 //order of spectrum
+lambda=5893*10^-8 //wavelength in cm
+//dtheta=2.5'=(2.5/60)*(3.14/180),we get
+dtheta=7.27*10^-4 //in radian
+dlambda=sqrt(((E/n)^2)-lambda^2)*dtheta
+disp("the difference in wavelengths of two lines is dlambda="+string(dlambda)+"cm")
diff --git a/2780/CH3/EX3.26/Ex3_26.sce b/2780/CH3/EX3.26/Ex3_26.sce new file mode 100755 index 000000000..86d6a3bc2 --- /dev/null +++ b/2780/CH3/EX3.26/Ex3_26.sce @@ -0,0 +1,6 @@ +clc
+//to calculate aperture of the objective of a telescope
+lambda=6*10^-5 //wavelength of light in cm
+dtheta=4.88*10^-6 // in radians
+a=1.22*lambda/dtheta
+disp("the aperture of the objective of a telescope is a="+string(a)+"cm")
diff --git a/2780/CH3/EX3.27/Ex3_27.sce b/2780/CH3/EX3.27/Ex3_27.sce new file mode 100755 index 000000000..164f6351a --- /dev/null +++ b/2780/CH3/EX3.27/Ex3_27.sce @@ -0,0 +1,8 @@ +clc
+//to calculate separation of two points on the moon
+lambda=5.5*10^-5 //wavelength of light in cm
+a=500 //diameter in cm
+dtheta=1.22*lambda/a //limit of resolution of telescope in radians
+R=3.8*10^8 //distance between earth and moon in m
+X=R*dtheta
+disp("the separation of two points on the moon is X="+string(X)+"m")
diff --git a/2780/CH3/EX3.28/Ex3_28.sce b/2780/CH3/EX3.28/Ex3_28.sce new file mode 100755 index 000000000..81426eb7e --- /dev/null +++ b/2780/CH3/EX3.28/Ex3_28.sce @@ -0,0 +1,6 @@ +clc
+//to calculate numerical aperture of the objective
+lambda=5.461*10^-5 //wavelength in cm
+S=5.55*10^-5 //distance in cm
+NA=1.22*lambda/(2*S)
+disp("the numerical aperture of the objective is NA="+string(NA)+"unitless")
diff --git a/2780/CH3/EX3.29/Ex3_29.sce b/2780/CH3/EX3.29/Ex3_29.sce new file mode 100755 index 000000000..c2c46ae20 --- /dev/null +++ b/2780/CH3/EX3.29/Ex3_29.sce @@ -0,0 +1,6 @@ +clc
+//to calculate resolving power of microscope
+NA=0.12 //numerical aperture
+lambda=6*10^-5 //wavelength of light in cm
+RP=2*NA/lambda //RP=resolving power
+disp("the resolving power of microscope is RP="+string(RP)+"unitless")
diff --git a/2780/CH3/EX3.3/Ex3_3.sce b/2780/CH3/EX3.3/Ex3_3.sce new file mode 100755 index 000000000..028baf7df --- /dev/null +++ b/2780/CH3/EX3.3/Ex3_3.sce @@ -0,0 +1,7 @@ +clc
+//to calculate width of slit
+//direction of minima in fraunhofer diffraction due to single slit is given by %pi/lambda*e*siuntheta=+m*%pi,where m=1,2,3
+//angular spread of the central maximum on either side of the incident light is sintheta=lambda/e,where m=1,position of first minima
+lambda=5000*10^-8
+e=lambda/sin(%pi/6)
+disp("width of slit is e="+string(e)+"cm")
diff --git a/2780/CH3/EX3.30/Ex3_30.sce b/2780/CH3/EX3.30/Ex3_30.sce new file mode 100755 index 000000000..50e707371 --- /dev/null +++ b/2780/CH3/EX3.30/Ex3_30.sce @@ -0,0 +1,10 @@ +clc
+//to calculate maximum resolving power
+lambda=5*10^-5 //wavelength of light in cm
+N=40000 //total number of lines on grating
+//(e+d)=12.5*10^-5 cm
+//formula is nmax=(e+d)/lambda
+//we get
+nmax=2 //order of spectrum
+RP=nmax*N //RP=resolving power
+disp("the maximum resolving power is RP="+string(RP)+"unitless")
diff --git a/2780/CH3/EX3.31/Ex3_31.sce b/2780/CH3/EX3.31/Ex3_31.sce new file mode 100755 index 000000000..13e11a5e8 --- /dev/null +++ b/2780/CH3/EX3.31/Ex3_31.sce @@ -0,0 +1,11 @@ +clc
+//to calculate minimum number of lines in a grating
+lambda1=5890
+ //wavelengh in angstrom
+lambda2=5896
+dlambda=6 //smallest wavelength difference in angstrom
+n=2 //order of spectrum
+lambda=(lambda1+lambda2)/2 //average wavelength in angstrom
+RP=lambda/dlambda //RP=resolving power
+N=RP/n
+disp("minimum number of lines in a grating is N="+string(N)+"unitless")
diff --git a/2780/CH3/EX3.32/Ex3_32.sce b/2780/CH3/EX3.32/Ex3_32.sce new file mode 100755 index 000000000..f82252368 --- /dev/null +++ b/2780/CH3/EX3.32/Ex3_32.sce @@ -0,0 +1,12 @@ +clc
+//will the telescope be able to observe the wiremesh
+a=3 //aperture in cm
+lambda=5.5*10^-5 //wavelength of light in cm
+//limit of resolution of telescope is given by
+theta=1.22*lambda/a
+//alpha=spacing of wire-mesh/distance of objective from wire-mesh
+alpha=0.2/(80*10^2)
+disp("theta="+string(theta)+"radian")
+disp("alpha="+string(alpha)+"radian")
+disp("if alpha>theta then telescope will be able to observe the wire-mesh")
+//value of alpha is given wrong in the book 2.25*10^-5 radian
diff --git a/2780/CH3/EX3.33/Ex3_33.sce b/2780/CH3/EX3.33/Ex3_33.sce new file mode 100755 index 000000000..cb8e73d45 --- /dev/null +++ b/2780/CH3/EX3.33/Ex3_33.sce @@ -0,0 +1,7 @@ +clc
+//distance between the centres of images of two stars
+lambda=5500*10^-8 //wavelength of light in cm
+f=4*10^2 //focal length of telescope objective in cm
+a=0.01*10^2 //diameter in cm
+X=1.22*lambda*f/a
+disp("distance between the centres of images of two stars is X="+string(X)+"cm ")
diff --git a/2780/CH3/EX3.34/Ex3_34.sce b/2780/CH3/EX3.34/Ex3_34.sce new file mode 100755 index 000000000..8935c88dd --- /dev/null +++ b/2780/CH3/EX3.34/Ex3_34.sce @@ -0,0 +1,6 @@ +clc
+//to calculate diameter of a telescope
+lambda=5*10^-5 //wavelength in cm
+theta=(%pi/180)*(1/1000) //in radians
+a=1.22*lambda/theta
+disp("the diameter of a telescope is a="+string(a)+"cm")
diff --git a/2780/CH3/EX3.35/Ex3_35.sce b/2780/CH3/EX3.35/Ex3_35.sce new file mode 100755 index 000000000..1eab6bc84 --- /dev/null +++ b/2780/CH3/EX3.35/Ex3_35.sce @@ -0,0 +1,6 @@ +clc
+//to calculate smallest angle between two stars
+lambda=5*10^-5 //wavelength in cm
+a=100*2.54 //diameter in cm
+theta=1.22*lambda/a
+disp("the smallest angle between two stars is thita="+string(theta)+"radians")
diff --git a/2780/CH3/EX3.36/Ex3_36.sce b/2780/CH3/EX3.36/Ex3_36.sce new file mode 100755 index 000000000..ec56327a0 --- /dev/null +++ b/2780/CH3/EX3.36/Ex3_36.sce @@ -0,0 +1,7 @@ +clc
+//to calculate limit of resolution of the telescope
+lambda=5890*10^-8 //wavelength in cm
+a=1 //diameter in cm
+theta=1.22*lambda/a
+disp("the limit of resolution of the telescope is theta="+string(theta)+"radians ")
+
diff --git a/2780/CH3/EX3.37/Ex3_37.sce b/2780/CH3/EX3.37/Ex3_37.sce new file mode 100755 index 000000000..f19c72e1a --- /dev/null +++ b/2780/CH3/EX3.37/Ex3_37.sce @@ -0,0 +1,6 @@ +clc
+//to calculate resolving limit of microscope
+lambda=5.5*10^-5 //wavelengh in cm
+theta=%pi/6 //in radians
+s=1.22*lambda/(2*sin(%pi/6))
+disp("resolving limit of microscope is s="+string(s)+"cm")
diff --git a/2780/CH3/EX3.38/Ex3_38.sce b/2780/CH3/EX3.38/Ex3_38.sce new file mode 100755 index 000000000..deb8bf540 --- /dev/null +++ b/2780/CH3/EX3.38/Ex3_38.sce @@ -0,0 +1,10 @@ +clc
+//to calculate resolving power of grating
+N=15000 //total number of lines on grating
+lambda=6*10^-5 //wavelength in cm
+n=2 //order of spectrum
+RP=n*N
+disp("resolving power is RP ="+string(RP)+"unitless")
+//to calculate smallest wavelength difference that can be resolved with a light of wavelength 6000angstrom in the second order
+dlambda=lambda/(n*N)
+disp("smallest wavelength difference dlambda="+string(dlambda)+"cm")
diff --git a/2780/CH3/EX3.39/Ex3_39.sce b/2780/CH3/EX3.39/Ex3_39.sce new file mode 100755 index 000000000..68015b87e --- /dev/null +++ b/2780/CH3/EX3.39/Ex3_39.sce @@ -0,0 +1,11 @@ +clc
+//to calculate resolving power in the second order
+N=6*10^4 //N=total number of lines on grating
+n=2 //order of spectrum
+RP=n*N //RP=resoling power
+disp("the resolving power is RP="+string(RP)+"unitless")
+//to calculate smallest wavelength
+lambda=6000*10^-8 //wavelength in cm
+n=3 //order of spectrum
+dlambda=lambda/(n*N)
+disp("smallest wavelength that can be resolved in the third order in 6000angstrom wavelength region is dlambda="+string(dlambda)+"cm")
diff --git a/2780/CH3/EX3.4/Ex3_4.sce b/2780/CH3/EX3.4/Ex3_4.sce new file mode 100755 index 000000000..0470048f3 --- /dev/null +++ b/2780/CH3/EX3.4/Ex3_4.sce @@ -0,0 +1,11 @@ +clc
+//to calculate wavelength of incident light
+//direction of minima is given by e*sintheta=+m*lambda
+//for first minima m=1,i.e. e*sintheta=lambda,sintheta is approximately equal to theta,then we can write it as e*theta=lambda ...........eq(1)
+//theta=Y/d........................eq(2)
+e=0.02 //in cm
+Y=0.5 //position of first minima from the central maxima in cm
+d=200 //distance of screen from the slit in cm
+//from eq(1) and eq(2),we get
+lambda=e*Y/d
+disp("wavelength of incident light is lambda="+string(lambda)+"cm")
diff --git a/2780/CH3/EX3.6/Ex3_6.sce b/2780/CH3/EX3.6/Ex3_6.sce new file mode 100755 index 000000000..1f564fca7 --- /dev/null +++ b/2780/CH3/EX3.6/Ex3_6.sce @@ -0,0 +1,16 @@ +clc
+//to calculate values of lambda1 and lambda2
+//in fraunhofer diffraction pattern ,the direction of minima is given by e*sintheta=+m*lambda,where m=1,2,.......
+//direction of fourth minima (m=4) for wavelength lambda1 is given by e*sintheta1=4*lambda1..........eq(1)
+//similarly, e*sintheta2=5*lambda2..........eq(2)
+//from eq(1) and eq(2),we get e*sintheta=4*lambda1=5*lambda2....eq(3)
+y=0.5 //in cm
+f=100 //in cm
+theta=y/f //in radian
+sintheta=theta //theta is very small
+e=0.05 //width of slit in cm
+lambda1=e*sintheta/4
+disp("lambda1="+string(lambda1)+"cm")
+//from eq(3) we get,
+lambda2=4*lambda1/5
+disp("lambda2="+string(lambda2)+"cm")
diff --git a/2780/CH3/EX3.7/Ex3_7.sce b/2780/CH3/EX3.7/Ex3_7.sce new file mode 100755 index 000000000..c6526d866 --- /dev/null +++ b/2780/CH3/EX3.7/Ex3_7.sce @@ -0,0 +1,6 @@ +clc
+//to calculate half angular width
+e=1.2*10^-4 //width of slit in cm
+y=6*10^-5 //wavelength of monochromatic light in cm
+theta=y/e
+disp("half angular width of central bright maxima is theta="+string(theta)+"radian")
diff --git a/2780/CH3/EX3.8/Ex3_8.sce b/2780/CH3/EX3.8/Ex3_8.sce new file mode 100755 index 000000000..6333c0dc1 --- /dev/null +++ b/2780/CH3/EX3.8/Ex3_8.sce @@ -0,0 +1,9 @@ +clc
+//to calculate angle
+lambda=6000*10^-8 //wavelength of light in cm
+e=0.03 //width of slit in cm
+//e*sintheta=m*lambda,where m=1
+theta=asind(lambda/e)
+disp("angle at which the first dark band are formed in the fraunhofer diffraction pattern is theta="+string(theta)+"degree")
+theta1=asind(3*lambda/(2*e))
+disp("angle at which the next bright band are formed in the fraunhofer diffraction pattern is theta1="+string(theta1)+"degree")
diff --git a/2780/CH3/EX3.9/Ex3_9.sce b/2780/CH3/EX3.9/Ex3_9.sce new file mode 100755 index 000000000..97256a692 --- /dev/null +++ b/2780/CH3/EX3.9/Ex3_9.sce @@ -0,0 +1,14 @@ +clc
+//to calculate distances of first dark band and of next bright band on either side of the central maximum
+//formula is e*sintheta=m*lambda,where m=1
+lambda=5890*10^-8 //wavelength of light in cm
+e=0.03 //width of slit in cm
+sintheta=lambda/e
+theta=sintheta //becoz theta is very small,so sintheta is approximately equal to theta
+f=50
+y=f*theta
+disp("linear distance of first minimum from the central maximum is y="+string(y)+"cm")
+sintheta1=3*lambda/(2*e)
+theta1=sintheta1
+y1=f*theta1
+disp("linear distance of first secondary maxima is y1="+string(y1)+"cm")
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