Waves and Modern Physics 203-SN3-RE • CEGEP, Montreal
Corrected practice final exam: waves and modern physics, with heat and climate (203-SN3-RE)
A chapter set announces its topic; a final exam does not, and that is the only difference that matters. This practice final covers 203-SN3-RE (formerly 203-NYC), Waves and Modern Physics, as defined by the revised Natural Science program (200.B1): oscillatory motion, wave phenomena, quantum and nuclear physics, and environmental issues treated through heat transfer and the radiative balance.
The four parts are worth 25 marks each. Unlike the practice final of the former 203-NYC course, this one contains no geometric optics and includes the block on heat, the greenhouse effect and radiative forcing. CEGEPs do not all schedule the course the same way: if yours keeps geometric optics, complete it with the exercise set devoted to that topic. Each exercise has its answer boxes checked on the page and a complete worked solution.
Exam advice: three hours, a calculator, and a formula sheet if your CEGEP allows one. Do the whole exam in one sitting before opening a single solution.
Self-checking setType your answers and check them question by question: the page tells you right or wrong before you open the solution. With an account, every answer right on the first try earns points, and your right answers stay filled in when you come back.
Exercise 1: The dancing washing machine: oscillator and resonance
The tub of a washing machine, of mass 40 kg with its laundry, rests on springs equivalent to a single spring of stiffness 1.6×104 N/m. Treat it as an undamped vertical harmonic oscillator.
a) Calculate the natural angular frequency of the oscillator.
b) Calculate its natural frequency.
c) The drum spins faster and faster during the spin cycle. At what rotation speed, in revolutions per minute, does the tub go into resonance?
d) The tub oscillates with an amplitude of 5.0 mm at its natural frequency. Calculate its maximum speed and its maximum acceleration.
e) Why do washing machines accelerate the drum quickly at the start of the spin cycle?
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Answers
a)ω0=20 rad/s
b)f0=3.18 Hz
c)191 rpm
d)vmax=0.10 m/s, amax=2.0 m/s²
e)Pass quickly through the resonance
a)
ω0=mk=401.6×104=20 rad/s.
b)
f0=2πω0=3.18 Hz. Confusing ω with f loses a factor of 2π, the most common error in the chapter.
c)
The unbalanced laundry drives the tub at the rotation frequency of the drum: resonance occurs when it equals 3.18 revolutions per second, that is 3.18×60=191 rpm.
d)
vmax=Aω0=0.0050×20=0.10 m/s and amax=Aω02=0.0050×400=2.0 m/s².
e)
At resonance, the amplitude would be limited only by damping and could become dangerous. By passing quickly through the range around 191 rpm on the way to 1000 rpm or more, the drive does not stay at the natural frequency long enough for the amplitude to build up.
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Exercise 2: Reading a travelling wave from its equation
A transverse wave travels along a string of linear mass density 0.050 kg/m. The displacement is y(x,t)=0.020sin(2.5x−40t), in SI units.
a) Calculate the wavelength.
b) Calculate the frequency.
c) Calculate the wave speed, and give the direction of propagation.
d) Calculate the maximum transverse speed of a point on the string.
e) Calculate the tension in the string.
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Answers
a)λ=2.51 m
b)f=6.37 Hz
c)v=16 m/s toward positive x
d)vy,max=0.80 m/s
e)T=12.8 N
a)
Wave number k=2.5 rad/m: λ=k2π=2.51 m.
b)
Angular frequency ω=40 rad/s: f=2πω=6.37 Hz.
c)
v=kω=2.540=16 m/s. The form sin(kx−ωt) travels toward POSITIVE x: a constant phase requires x to increase as t increases.
d)
vy=∂t∂y=−0.020×40cos(2.5x−40t), with maximum Aω=0.80 m/s, twenty times smaller than the wave speed: two speeds that must never be confused.
e)
v=μT, so T=μv2=0.050×162=12.8 N.
Exercise 3: The violin string: standing waves and emitted sound
The A string of a violin vibrates between two fixed points 33.0 cm apart. Its fundamental frequency is 440 Hz and its linear mass density is 0.60 g/m. Speed of sound in air: 343 m/s.
a) Calculate the wave speed on the string.
b) Calculate the tension in the string.
c) Calculate the frequency of the third harmonic.
d) Calculate the wavelength of the 440 Hz sound in air.
e) The violinist presses the string down a third of the way along it, leaving only the remaining two thirds free to vibrate. What note, in Hz, does the violinist get?
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Answers
a)v≈290 m/s
b)T≈50.6 N
c)1320 Hz
d)λair=0.780 m
e)660 Hz
a)
Fundamental of a string fixed at both ends: L=2λ1, so λ1=0.660 m and v=λ1f1=0.660×440=290 m/s.
b)
T=μv2=0.60×10−3×290.42=50.6 N. The linear mass density must be in kg/m.
c)
f3=3f1=1320 Hz.
d)
The FREQUENCY is conserved in passing from the string to the air, while the wavelength changes with the speed: λair=440343=0.780 m, whereas it is 0.660 m on the string.
e)
The tension and the linear mass density do not change, so neither does v; the vibrating length becomes 32L: f=2⋅32Lv=23×440=660 Hz, a perfect fifth above.
Part B: wave optics (/25)
Exercise 4: The diffraction grating and the hydrogen lines
A grating of 600 lines per millimetre is illuminated at normal incidence with the light of a hydrogen lamp, which contains in particular the lines at 486.1 nm (blue) and 656.3 nm (red). The maxima satisfy dsinθ=mλ. The diagram below defines the angle θ, measured from the normal to the grating; it is not to scale.
a) Calculate the grating spacing, in µm.
b) Calculate the angle of the blue line in first order.
c) Calculate the angle of the red line in first order.
d) What is the highest order observable for the red line?
e) Calculate the angle of the red line in that order.
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Answers
a)d=1.667 µm
b)17.0°
c)23.2°
d)Order 2
e)52.0°
a)
d=6001mm=1.667×10−6 m =1.667 µm.
b)
sinθ=1.667×10−6486.1×10−9=0.2917, so θ=17.0°.
c)
sinθ=1.667×10−6656.3×10−9=0.3938, so θ=23.2°. Red is deviated more than blue: the opposite of a prism.
d)
We need sinθ=dmλ≤1, that is m≤λd=2.54: order 2 is the last one.
e)
sinθ=1.667×10−62×656.3×10−9=0.7876, so θ=52.0°. The higher the order, the farther apart the lines are: the dispersion increases.
Exercise 5: The Rayleigh criterion: headlights, eye and telescope
Two point sources are just resolved by an instrument with a circular aperture of diameter D when their angular separation equals θmin=1.22Dλ. Take λ=550 nm.
a) Calculate the limiting angle of resolution of an eye with a 3.0 mm pupil, in rad.
b) The headlights of a car are 1.5 m apart. Out to what distance can the eye see them as separate, in km?
c) Calculate the limiting angle of an amateur telescope of 200 mm diameter.
d) What is the size of the smallest detail this telescope can distinguish on the Moon, at 3.84×105 km, in km?
e) Why does increasing the magnification of a telescope not let you see details finer than this limit?
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Answers
a)2.24×10−4 rad
b)L≈6.7 km
c)3.36×10−6 rad
d)s≈1.3 km
e)Diffraction limit
a)
θmin=1.22×3.0×10−3550×10−9=2.24×10−4 rad, or about 0.8 arcminute.
b)
For small angles, θ=Ls: L=2.24×10−41.5=6.7×103 m =6.7 km. Beyond that, the two headlights merge into a single blob.
c)
θmin=1.22×0.200550×10−9=3.36×10−6 rad, sixty-seven times better than the eye.
d)
s=Lθ=3.84×108×3.36×10−6=1.29×103 m =1.3 km.
e)
The limit comes from DIFFRACTION by the aperture: each point of the object gives a spot whose angular size is set by Dλ. Magnifying enlarges the spots as much as their separation, without separating them any further. Only a larger diameter, or a shorter wavelength, improves the resolution.
Exercise 6: Liquid crystal displays and polarizing glasses
The light from a liquid crystal display leaves linearly polarized, with an intensity of 400 W/m² along the axis (a made-up value, chosen for the calculations). Malus's law: I=I0cos2θ, where θ is the angle between the polarization and the axis of the polarizer. An ideal polarizer illuminated with UNPOLARIZED light transmits half of it.
a) A user wears polarizing glasses whose axis makes an angle of 60° with the polarization of the screen. What intensity reaches the user?
b) The user tilts their head until the axis is at 90°. What intensity reaches them?
c) Between the screen and the glasses at 90°, we insert a polarizer whose axis makes an angle of 45° with the polarization of the screen. What intensity now passes through the glasses?
d) Unpolarized light from the sky reaches the glasses with an intensity of 300 W/m². What intensity is transmitted?
e) Why does adding a filter in part c) INCREASE the transmitted light?
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Answers
a)100 W/m²
b)0
c)100 W/m²
d)150 W/m²
e)The filter redefines the polarization
a)
I=400cos260°=400×0.25=100 W/m².
b)
cos90°=0: no light at all, the screen looks black.
c)
First filter at 45°: 400cos245°=200 W/m², now polarized at 45°. The glasses make an angle of 90°−45°=45° with this new polarization: 200cos245°=100 W/m².
d)
In unpolarized light, all directions are equally present and the average of cos2θ is 21: 150 W/m².
e)
A polarizer does not merely BLOCK part of the light: it REDEFINES the polarization of what it lets through. The intermediate filter rotates the polarization by 45°, which gives the glasses a nonzero component to transmit. Without it, the polarization of the screen was exactly perpendicular to the glasses.
Part C: modern physics (/25)
Exercise 7: Measuring Planck's constant with two stopping potentials
A metal cathode is illuminated in turn with two monochromatic lights and we measure the stopping potential Vs that cancels the photoelectric current: Vs=1.87 V for λ=300 nm and Vs=0.84 V for λ=400 nm. Einstein's relation: eVs=hf−W. e=1.60×10−19 C, c=3.00×108 m/s.
a) Calculate the two frequencies, in 1014 Hz.
b) Deduce Planck's constant from the two measurements.
c) Calculate the work function of the metal, in eV.
d) Calculate the threshold wavelength, in nm.
e) The intensity of the 300 nm light is doubled. What happens to the stopping potential?
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Answers
a)f1=10.0; f2=7.50 (×1014 Hz)
b)h≈6.59×10−34 J·s
c)W=2.25 eV
d)λ0≈549 nm
e)Unchanged
a)
f1=300×10−93.00×108=10.0×1014 Hz and f2=400×10−93.00×108=7.50×1014 Hz.
b)
Subtracting the two relations, W drops out: e(Vs1−Vs2)=h(f1−f2), so h=2.50×10141.60×10−19×1.03=6.59×10−34 J·s, within 0.5 % of the accepted value. This is the slope of the line Vs(f), multiplied by e.
λ0=Whc=3.60×10−196.59×10−34×3.00×108=5.49×10−7 m =549 nm: beyond that, in the yellow and red, no more electrons are emitted.
e)
It does not change: Vs measures the MAXIMUM kinetic energy of the electrons, which is set by the frequency. Doubling the intensity doubles the number of photons, and therefore the saturation current, not the energy of each electron.
Exercise 8: One photon absorbed, six lines emitted
Hydrogen atoms in their ground state are illuminated with ultraviolet light. Energy levels: En=−n213.6 eV; hc=1240 eV·nm. Photons of 97.3 nm are observed to be absorbed.
a) Calculate the energy of a 97.3 nm photon.
b) Which level does this photon raise the electron to?
c) On falling back to the ground state by every possible path, how many different lines can the atom emit?
d) Calculate the longest wavelength emitted, in nm.
e) In which region does this line lie?
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Answers
a)E=12.74 eV
b)n=4
c)6 lines
d)λ≈1.88×103 nm
e)Infrared (Paschen series)
a)
E=97.31240=12.74 eV.
b)
En=−13.6+12.74=−0.86 eV, so n2=0.8613.6≈16 and n=4. Check: 13.6(1−161)=12.75 eV.
c)
The possible transitions among levels 1 to 4 are 4→3, 4→2, 4→1, 3→2, 3→1, 2→1: six lines, 24×3 pairs of levels.
d)
The longest wavelength corresponds to the smallest energy gap, 4→3: ΔE=13.6(91−161)=0.661 eV and λ=0.6611240=1.88×103 nm.
e)
1876 nm is in the INFRARED: it is the first line of the Paschen series. An atom illuminated with ultraviolet light can re-emit in the infrared and in the visible (the 3→2 transition gives the 656 nm red line).
Exercise 9: The tritium in a glowing exit sign
Some emergency exit signs glow without electricity: tritium (3H, atomic mass 3.016 u), a beta emitter with a half-life of 12.3 years, excites a luminescent coating. A new sign has an activity of 3.7×1011 Bq. 1 u =1.6605×10−27 kg; 1 year =3.156×107 s.
a) Calculate the decay constant, in s⁻¹.
b) Calculate the number of tritium nuclei in the new sign.
c) Calculate the corresponding mass of tritium, in mg.
d) The brightness is proportional to the activity. What fraction of its initial brightness does the sign retain after 20 years, in %?
e) After how many years does the brightness fall to one quarter?
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Answers
a)λ=1.79×10−9 s⁻¹
b)N=2.07×1020
c)m≈1.04 mg
d)32 %
e)24.6 years
a)
λ=T1/2ln2=12.3×3.156×1070.693=1.79×10−9 s⁻¹. The half-life must be in SECONDS for an activity in becquerels.
b)
A=λN, so N=1.79×10−93.7×1011=2.07×1020 nuclei.
c)
m=2.07×1020×3.016×1.6605×10−27=1.04×10−6 kg =1.04 mg: about one milligram is enough.
d)
A0A=2−t/T1/2=2−20/12.3=0.324, that is 32 %.
e)
One quarter corresponds to two half-lives: 24.6 years. It can be read off without a logarithm, because 41=(21)2.
Part D: heat and climate (/25)
Exercise 10: The cooler: conduction and latent heat
A polystyrene cooler (k=0.033 W/(m·K)) has a wall area of 0.80 m² and a wall thickness of 3.0 cm. It contains ice at 0 °C; the outside air is at 30 °C. Neglect the resistance of the air films. Latent heat of fusion of ice: 3.34×105 J/kg.
a) Calculate the heat flow entering the cooler.
b) Calculate the mass of ice that melts in one hour, in g.
c) How long does 5.0 kg of ice last, in hours?
d) With walls 6.0 cm thick, what becomes of the heat flow?
e) Why does the temperature inside stay at 0 °C as long as ice remains?
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Answers
a)Φ=26.4 W
b)285 g per hour
c)About 17.5 h
d)13.2 W
e)Melting plateau at 0 °C
a)
Φ=ekAΔT=0.0300.033×0.80×30=26.4 W.
b)
In one hour, 26.4×3600=9.50×104 J enters, which melts 3.34×1059.50×104=0.285 kg =285 g.
c)
0.2855.0=17.5 h.
d)
The thermal resistance doubles and the heat flow is halved: 13.2 W, and the ice lasts twice as long.
e)
The energy that comes in goes into the CHANGE OF STATE, not into raising the temperature: as long as melting is not complete, the ice-water mixture stays at 0 °C. This is what makes ice so effective, and it is also what keeps the 30 K difference constant in the calculation.
Exercise 11: The temperature of an exoplanet
An exoplanet orbits at 0.80 AU (astronomical units) from a star half as luminous as the Sun. Its albedo is 0.35. At 1 AU from the Sun, the solar constant is 1361 W/m². σ=5.67×10−8 W/(m²·K⁴).
a) Calculate the stellar flux received at the distance of the planet.
b) Calculate its radiative equilibrium temperature, in K.
c) Express this temperature in °C.
d) With an atmosphere opaque to infrared, modelled as a single layer, Ts=21/4Te. Calculate the surface temperature, in °C.
e) Is liquid water possible at the surface in this second case?
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Answers
a)S≈1063 W/m²
b)Te≈235 K
c)−38 °C
d)Ts≈6 °C
e)Yes, thanks to the greenhouse effect
a)
The flux varies as d2L: S=1361×0.8020.5=1063 W/m².
b)
Te=(4σ(1−0.35)×1063)1/4=235 K.
c)
235−273=−38 °C.
d)
Ts=1.189×235=279 K, that is 6 °C.
e)
Yes: between 0 and 100 °C under sufficient pressure, water can be liquid. It is the greenhouse effect, and not the distance to the star alone, that decides habitability here: with no atmosphere, the same planet would be frozen.
Exercise 12: Forcing, climate sensitivity and observed warming
Radiative forcing of CO₂: ΔF=5.35lnC0C W/m², with C0=280 ppm. Take an equilibrium climate sensitivity s=0.80 K per W/m², feedbacks included: ΔTeq=sΔF.
a) Calculate the forcing of a doubling of CO₂.
b) Calculate the corresponding equilibrium warming.
c) Calculate the forcing of CO₂ at 420 ppm.
d) Calculate the equilibrium warming associated with this forcing.
e) The warming observed since the preindustrial era is about 1.2 K. Why is it lower than the value in d)?
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Answers
a)3.71 W/m²
b)3.0 K
c)2.17 W/m²
d)1.7 K
e)Ocean inertia and aerosols
a)
ΔF2×=5.35ln2=3.71 W/m².
b)
ΔTeq=0.80×3.71=3.0 K.
c)
ΔF=5.35ln280420=2.17 W/m².
d)
ΔTeq=0.80×2.17=1.7 K.
e)
Two main reasons. The thermal inertia of the ocean: the climate takes years to centuries to reach equilibrium, and part of the warming due to past emissions is still to come. Pollution aerosols, which raise the albedo and exert a negative forcing, mask part of the effect of the greenhouse gases. Other gases (methane), on the other hand, add their forcing to that of CO₂.
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