Past exam of the physics course of the year 1 of the natural sciences course of the University of Cambridge / 2014 / Paper 1

Original paper: Public original PDF, physical pages 23–33; cover on page 23, blank page 24 and questions on pages 25–33.

Each photon has energy $hf$, giving the photon emission rate from monochromatic power and wavelengthHere $P$ is radiated signal power, not the phone's total electrical consumption.

For this equal-mass Coulomb circular orbit, let $s$ be the separation and $k_e=1/(4\pi {ϵ}_0)$. Each particle describes a circle of radius $s/2$ about the centre of mass. Coulomb's law and centripetal acceleration giveUsing $s$ as each particle's orbital radius would miss the equal-mass two-body motion.

Use $[\eta ]=M{L}^{-1}{T}^{-1}$ and $[dp/dx]=M{L}^{-2}{T}^{-2}$. Equating mass, length and time exponents giveshenceDimensional analysis leaves $k$ undetermined. If positive $Q$ denotes flow along increasing $x$, the signed pressure derivative is negative and its minus sign belongs in the proportionality constant; alternatively use the pressure-drop magnitude.

Converting all lengths to metres gives $d=3.7276\times 10^{-5}\mathrm{m}$. Logarithmic differentiation givesIf the quoted uncertainties are independent standard uncertainties, monomial uncertainty propagation givesIf the quoted uncertainties instead mean bounds, the first-order conservative fractional error is $0.111$, giving approximately $37.3\pm 4.1\mu \mathrm{m}$. The question does not specify their statistical meaning; these two error conventions should not be combined.

For the real object and real image, take positive distances $u=f+u^{\prime }$ and $v=f+v^{\prime }$. The thin lens equation yieldsThis is Newton's lens formula. The distances $u^{\prime },v^{\prime }$ refer to the adjacent focal points, not the lens plane.

The total ring mass is $M=2\pi r{\lambda }_m=1.257\times 10^7\mathrm{kg}$. For the axial gravitational field of a uniform ring, transverse force components cancel by symmetry; each axial component has projection factor $z/\sqrt{r^2+z^2}$. ThusThe force points towards the ring's centre along its axis.

Take $q=\ddot{x}$ positive when the hanging mass descends and the other mass moves uphill. For the sliding block, Newton's second law gives $mg-T=mq$ and $T-Mg\sin \theta =Mq$. ThereforeFor the pulley coupled to a rolling disc, tension and weight act through its centre; the contact normal is perpendicular to the slope. Static friction provides the torque required for rolling without slipping. Define signed $F$ down the slope, so $F>0$ for uphill acceleration.

The rotational equation and rolling constraint give $Fa=Iq/a$, hence $F=Mq/2$. The translational equations become $T-Mg\sin \theta -F=Mq$ and $mg-T=mq$, givingThus the threshold remains $m>M\sin \theta$: the moment of inertia increases the effective mass but does not change the sign of the driving force. For downhill acceleration $F$ reverses. The normal force is $Mg\cos \theta$; static friction does no work at the stationary contact point and sufficient roughness is assumed.

In standard configuration the frames are inertial, their corresponding axes are parallel, S${}^{\prime }$ moves at $v$ along the positive $x$ axis of S, and their origins coincide at $t=t^{\prime }=0$. Here $(t,x,y,z)$ and $(t^{\prime },x^{\prime },y^{\prime },z^{\prime })$ label the same event, $c$ is the speed of light and $\gamma =(1-v^2/c^2{)}^{-1/2}$.

A clock fixed in S${}^{\prime }$ has $\Delta x^{\prime }=0$. The inverse time transformation givesso the moving clock accumulates less proper time between its two ticks than the elapsed S-coordinate time.

Without time dilation the flight time from the given altitude would be $66.7\mu \mathrm{s}$, about $30.3$ rest-frame mean lifetimes, giving survival fraction only $e^{-30.3}\simeq 6.8\times 10^{-14}$ even at speed $c$. Relativistic muons can instead reach the ground with appreciable survival. Momentum-selected decay measurements test this clock-rate dependence experimentally.^[ref]

A mean-lifetime survival energy estimate requires a mean flight time no greater than the dilated mean lifetime:This corresponds to survival probability at least about $e^{-1}$. There is no sharp minimum energy for an individual random decay. For a required probability $p$, use $\exp [-H/(\gamma v{\tau }_0)]\ge p$. Energy loss in the atmosphere is neglected in this estimate. In the muon's frame the atmospheric path is length-contracted to $H/\gamma \simeq 660\mathrm{m}$; the ground reaches it in about ${\tau }_0$, giving the same survival probability.

For the two-body decay, use the rest frame of A. Momentum conservation makes B and the photon oppositely directed with equal momentum magnitude $p$. Energy conservation and the energy–momentum relation giveSubstitution and cancellation of $E_B^2$ giveA nonzero emitted photon requires $m_A>m_B$.

About a specified axis, the moment of inertia is $I=\int r_{\perp }^{2}dm$, giving rotational kinetic energy $I{\omega }^2/2$ for fixed-axis rotation. With square coordinates centred on the plate,The in-plane inertia isotropy of a square plate follows using the perpendicular axis theorem, which gives $I_z=I_x+I_y=M{l}^2/6$. For any in-plane central axis at angle $\varphi$, the perpendicular in-plane axis has the same inertia by the square's $90^{\circ }$ rotational symmetry. Their sum is $I_z$, so every such in-plane axis has $I=M{l}^2/12$.

The parallel axis theorem gives hinge inertia $I_H=M{l}^2/3$. During the short impulse gravity is negligible, and the hinge impulse has no moment about the hinge. ThereforeThe hinge impulse of an edge-pivoted square plate follows from linear momentum: $J_H=Mv-K$. Taking its positive direction to be that of the applied impulse,Generally $K$ alone does not supply the centre-of-mass momentum compatible with rotation about the fixed hinge, so the hinge supplies the difference. Its impulse vanishes at the centre of percussion,

For sinusoidal steady state with convention $e^{i\omega t}$, complex impedance is the voltage phasor divided by the current phasor. Its modulus is the amplitude ratio and its argument is the voltage-current phase difference. Since $V_L=LdI/dt$,The original circuit is a series RLC circuit with output across the inductor. Its transfer function isFor the original capacitance, the outputs are $10.15\mathrm{mV}$ at $9\mathrm{MHz}$ and $4.65\mathrm{mV}$ at $10\mathrm{MHz}$, a ratio $0.458$. The current resonance is $f_0=1/(2\pi \sqrt{LC})=8.967\mathrm{MHz}$, so the circuit favors the first transmitter.

The resistor voltage is in phase with the current; the inductor voltage leads it by $\pi /2$ and the capacitor voltage lags by $\pi /2$. Large reactive voltages therefore nearly cancel in their phasor sum. A large inductor voltage is consistent with a small supply voltage: it is inductor voltage magnification, not power gain in a passive circuit.

Reducing the capacitance raises $f_0$ to $9.452\mathrm{MHz}$, between the two transmitters. Direct evaluation gives $7.02\mathrm{mV}$ and $7.22\mathrm{mV}$, respectively. Their similar detunings give approximately equal amplitudes; they are not exactly equal, partly because the numerator of $H$ also depends on frequency.

The two-tone output of a linear resonant circuit, for coherent monochromatic sources of equal input amplitude and arbitrary fixed input phases, isWith $A\simeq B=V_o$, this is approximatelyThus a $9.5\mathrm{MHz}$ rapid oscillation has a beat envelope repeating in magnitude at $1\mathrm{MHz}$. The signed envelope cosine has frequency $0.5\mathrm{MHz}$. Unequal amplitudes leave a small nonzero envelope minimum; independently drifting transmitter phases make the beating drift. No new frequency is generated by this ideal linear circuit.

For the spring oscillator,so the total mechanical energy is conserved.

For U-tube liquid oscillation, define positive $y$ as the fall of the left surface, equal to the rise of the right surface. The hydrostatic height difference is $2y$. Moving a volume $Ady$ against this height difference gives $dU=2\rho gAydy$, henceEnergy conservation yields $\rho Al\dot{y}(\ddot{y}+2gy/l)=0$. Equivalently the net pressure force is $-2\rho gAy$, so the equation holds also at turning points:With negligible added volume, $y(0)=0$, $\dot{y}(0)=0.015\mathrm{m}{\mathrm{s}}^{-1}$. ThusThe graph starts at zero with positive slope and first reaches its maximum after $T/4$.

For viscously damped U-tube oscillation, the total damping force is $-\beta l\dot{y}$, not $-\beta \dot{y}$. ConsequentlyThe underdamped initial-value solution is $y=(v_0/{\omega }_d)e^{-\Gamma t/2}\sin {\omega }_{d}t$, where ${\omega }_d=\sqrt{{\omega }_0^2-{\Gamma }^2/4}=6.255{\mathrm{s}}^{-1}$. Setting its amplitude envelope equal to $0.1\mathrm{mm}$ givesThis is the decay of the envelope, not the first time the instantaneous displacement passes through $0.1\mathrm{mm}$.

A travelling wave, for example $A\cos (kx-\omega t)$, has moving constant-phase surfaces. A standing wave, for example $2A\sin (kx)\cos (\omega t)$, has stationary nodes and can be formed from two equal counterpropagating waves.

For the half-line finite well with $E>V_0$, define $k=\sqrt{2mE}/\hslash$ and $q=\sqrt{2m(E-V_0)}/\hslash$. The hard wall requires $\psi =0$ for $x<0$ and $\psi (0)=0$, so the general allowed forms areAt the finite step both $\psi$ and ${\psi }^{\prime }$ are continuous:There is no requirement to match the derivative to zero across the infinite wall.

For a bound state $0<E<V_0$, put $\kappa =\sqrt{2m(V_0-E)}/\hslash >0$. Normalizability excludes the growing exponential, leaving $A\sin (kx)$ inside and $D{e}^{-\kappa (x-a)}$ outside. Matching their logarithmic derivatives givesThe exterior expression is equivalent to $C{e}^{-\kappa x}$ by rescaling its constant. Negative cotangent first occurs for $\pi /2<ka<\pi$; all higher allowed intervals also have $ka>\pi /2$. Thus ${\lambda }_1=2\pi /k<4a$. Since $k<\sqrt{2m{V}_0}/\hslash$, a normalizable bound state requiresThis is also sufficient: on the lowest negative-cotangent branch, the two matching sides cross whenever $a\sqrt{2m{V}_0}/\hslash >\pi /2$. The printed non-strict inequality includes the threshold limit. At equality $E=V_0$ and the exterior is not square-integrable, so it is not itself a bound state.

For the helium mass and energy scale given, the limiting width isActual binding requires a width just larger than this threshold in the stated ideal potential.

Represent each wave by a complex phasor. Add phasors before squaring: two amplitudes give $I\propto |A_1+A_2{e}^{i\delta }{|}^2=A_1^2+A_2^2+2A_1{A}_2\cos \delta$. For $N$ equally illuminated narrow slits, adjacent phasors differ by $\delta =2\pi d\sin \theta /\lambda$, soAll phasors align when $\delta =2\pi m$, giving the grating equationThe nearest zero has adjacent-phase increment $2\pi /N$: the phasor polygon closes once. Thus $d\cos {\theta }_m\Delta \theta \simeq \lambda /N$, givingThe angular linearization is valid away from grazing directions; the underlying exact first-zero condition is $d(\sin {\theta }_{\mathrm{zero}}-\sin {\theta }_m)=\pm \lambda /N$.

For the first subsidiary maximum of a large slit array, use the stipulated $1.5$ phasor wraps: $N\delta /2\simeq 3\pi /2$ relative to a principal maximum. Its amplitude is approximately $2N/(3\pi )$ times one slit's amplitude. ThereforeThis uses the question's approximate maximum position, not the exact extremum of the slit-array intensity.

The Rayleigh criterion places one line's principal maximum at the other's first minimum. Grating dispersion then gives $|m|N\gtrsim \lambda /\delta \lambda =1.674\times 10^6$. Combining with normal incidence, $|m|\lambda =d|\sin \theta |$, gives the normal-incidence grating width bound:The $1.29\mathrm{m}$ value is an ideal lower bound approached near grazing diffraction. A usable finite angle needs greater width; for example $\theta =60^{\circ }$ requires about $1.49\mathrm{m}$. The exact sine first-zero relation still gives the lower bound when the local angular approximation fails near grazing.

Such a coherently illuminated grating is very large and needs accurate groove placement and suitable collection optics; an unaided far-field screen would require distances much greater than $W^2/\lambda \sim 2\times 10^6\mathrm{m}$. Focusing optics avoid that screen distance but not the required resolving power of a diffraction grating. Real linewidth, slit width and aberrations can require more resolution. The unequal isotope abundances also make this ideal Rayleigh estimate less decisive than for equally bright lines.

An inverse-square field spreads through area proportional to squared distance. More generally the flux contribution of a point source is proportional to the solid angle subtended by a surface element; the oriented solid angles sum to $4\pi$ for an enclosed source and zero for an exterior one. Superposition extends this to a mass distribution.

Newton's law of universal gravitation gives $\mathbf{g}=-GM\hat{\mathbf{r}}/r^2$ for a point mass. A surrounding sphere therefore has flux $-4\pi GM$, soFor the tunnel, approximate its water as an infinite uniform cylinder with $R=3.5\mathrm{m}$ and density $\rho =1000\mathrm{kg}{\mathrm{m}}^{-3}$. The bob is at radial distance $r=R+1.5\mathrm{m}=5.0\mathrm{m}$. A coaxial Gaussian surface givesFor the plumb-line deflection from cylindrical gravity, horizontal equilibrium gives $d/L\simeq |g_r|/g$. Draining removes the attraction toward the tunnel, so the bob shifts away byThe unchanged rock and ordinary gravitational field cancel in the before/after comparison; end effects and mechanical disturbances are neglected.

For the tidal water loading of a spring balance, approximate the extra water at high tide as an infinite plane slab of thickness $h=8\mathrm{m}$, with the suspended mass above it. The gravitational field of an infinite plane sheet, derived with a pillbox Gaussian surface, gives added downward field $\Delta g=2\pi G\rho h$. With initial spring extension $x_0=mg/k=1\mathrm{m}$,The extension increases at high tide. These estimates use $g=9.81\mathrm{m}{\mathrm{s}}^{-2}$ and the stated water-density approximation; salinity, finite estuary geometry and terrestrial tidal deformation alter a real measurement.

A field assigns a physical quantity to each point. Gravitational field is force per unit test mass; electric field is force per unit test charge. In a conservative, time-independent field,Write $U=m\Phi$ for gravitational potential $\Phi$, or $U=q\varphi$ for electric potential $\varphi$, giving $\mathbf{g}=-\nabla \Phi$ and $\mathbf{E}=-\nabla \varphi$. A point mass has $U=-GMm/r$ with zero at infinity, while two point charges have $U=Qq/(4\pi {ϵ}_{0}r)$. Only potential-energy differences matter; a constant can be added freely. The mechanical energy $K+U$ is conserved if no nonconservative forces do work. A magnetic Lorentz force $q\mathbf{v}\times \mathbf{B}$ does no work on a point charge and generally cannot be represented by a position-only scalar potential energy.

Faraday's law relates induced electromotive force to the rate of change of magnetic flux linkage. For a coil with $N$ turns and a consistent right-hand orientation,Flux can change through field variation or circuit motion. Lenz's law is the minus sign: the induced current's field opposes the flux change, consistent with energy conservation. It opposes the change rather than necessarily opposing the original field.

For a linear fixed-geometry inductor, $N{\Phi }_B=LI$ and the self-induced electromotive force is $-LdI/dt$. The passive terminal voltage drop is instead $V=LdI/dt$. The stored magnetic energy isInductance is measured in henries. Transformers use mutual inductance: changing one winding's current induces an electromotive force in another.

For steady currents in vacuum, the Biot-Savart law sums the contributions of current elements:It is useful for known wire geometries; a circular loop of radius $a$ gives $B={\mu }_{0}I/(2a)$ at its centre.

Ampère's circuital law in magnetostatics isWith sufficient symmetry it finds fields directly: a long straight wire gives $B={\mu }_{0}I/(2\pi r)$, while a long solenoid has interior $B\simeq {\mu }_{0}nI$ and a small exterior field away from its ends. Without symmetry, a circulation value alone does not determine the local field. For time-dependent electric fields, use the Ampère-Maxwell equation with the displacement-current term ${\mu }_0{ϵ}_{0}d{\Phi }_E/dt$ as well as conduction current.

For a test mass moving around a fixed central mass $M$, gravity is central and conservative. Specific angular momentum $h=|\mathbf{r}\times \mathbf{v}|$ and specific orbital energy $ϵ=v^2/2-GM/r$ are constant. The motion is planar and sweeps equal areas in equal times, $dA/dt=h/2$.

For a nonradial orbit, the inverse-square force gives a conic section,Negative energy gives an ellipse, zero energy a parabola and positive energy a hyperbola. For an ellipse of semimajor axis $a$,A circular orbit is the $e=0$ case, with $v=\sqrt{GM/r}$. Escape from radius $r$ requires $v\ge \sqrt{2GM/r}$ in the absence of further forces. For two comparable masses, apply the relative two-body equation with $GM$ replaced by $G(M+m)$, rather than treating one body as fixed.