The collection

Every essay — page 26

One idea per essay, ordered so that the earlier ones set up the later ones — but nothing here depends on being read in sequence.

Mechanics

Motion, force, and the quantities that refuse to change.

Waves

Oscillation, and everything that turns out to be an oscillation.

Optics

Light, and the small number of rules it obeys.

Electromagnetism

Charge, field, and the lines drawn between them.

London's attraction, and the distance where it gives out. The dispersion energy between two identical atoms times the sixth power of their separation, relative to London's constant, against the separation in units of c/ω₀ — the reduced wavelength of each atom's strongest transition — on logarithmic axes, from the Casimir–Polder integral with a one-resonance polarisability. Close in, the product is one: London's inverse sixth power. It has fallen to a half by 3.82 c/ω₀, and far out it falls as one over the distance, so the energy goes as the inverse seventh power, reaching 23.2 per cent of London's value at ten reduced wavelengths and 2.44 per cent at a hundred. For two helium atoms, whose strongest line is at 58 nm, c/ω₀ is about 9 nm; for two sodium atoms, 94 nm.

The attraction that weakens when light is too slow

Two neutral atoms attract because each one's fluctuating electrons polarise the other, and the two fluctuations fall into step. London's calculation of the force, as the inverse sixth power of the distance, assumes the field from one atom reaches the other instantly. It does not. Beyond a distance set by the wavelength of the atoms' own strongest transition — nine nanometres for helium, about a hundred for sodium — the field returns too late to find the fluctuation that made it. The attraction then falls one power faster. Casimir and Polder worked this out in 1948, and it was the starting point for the Casimir force between plates.

5 figures · part 5 on Retardation
Four places where three charges' fields cancel. Field lines in the plane of three equal positive point charges at the corners of an equilateral triangle, with every point where the field is zero marked. There are four: one at the centre, and three more on the lines from the centre to the middle of each side, 0.164 of a side from the centre. Four is (n − 1)² for three charges, the largest number Maxwell conjectured any three charges could make. Each zero is a saddle: along some directions the field pushes a test charge back and along others away, so none of them can hold anything still.

The zeros a handful of charges can make

Between two equal charges there is a point where their fields cancel. With three there can be two such points, or one, or four. Every such point is a saddle, never a place where a charge could rest. In two dimensions the count is fixed by algebra: n equal line charges make exactly n − 1 zeros, the roots of a polynomial's derivative. In three dimensions nobody knows the answer. In 1873 Maxwell conjectured that n point charges can make at most (n − 1)² zeros. Three charges on a triangle make exactly four, and the conjecture has not been proved even for three charges.

5 figures · part 5 on The field concept
How much reflected light keeps its handedness. Circularly polarised light reflected from a flat surface: the fraction of the reflected power that keeps its handedness, against the angle of incidence, for a perfect conductor, for glass, n = 1.5, for a medium with ε = μ = 1.5 (the same index, and the same impedance as empty space), and for one in between. A metal mirror reverses the handedness of every photon at every angle. Glass reverses it at normal incidence, returns an even split at Brewster's angle (56.3°, where only one linear polarisation reflects), and keeps 60 per cent at 60°. The medium with ε = μ keeps it at every angle: it respects the duality symmetry, and so conserves what the symmetry conserves.

The handedness a mirror cannot keep

Maxwell's equations in empty space do not change if the electric field is turned partly into the magnetic field and the magnetic partly into the electric. A symmetry that exact must hand over a conserved quantity, and this one hands over the handedness of light — how many more photons spin one way than the other. Every mirror breaks it: circularly polarised light comes back from a mirror with its handedness reversed. Only a material that responds to the magnetic field exactly as strongly as to the electric one keeps it, and such a material, it turns out, sends nothing straight back.

5 figures · part 5 on Maxwell equations
Two pieces of current that one law makes push each other unequally. Two short elements of current a unit distance apart: element 1 pointing along the line joining them, element 2 at 45° to it. Left, the forces by the law that follows from Biot and Savart (Grassmann's): element 1 pushes nothing on element 2, because 1 points straight at it, while element 2 pushes on element 1 with a force of 0.71 units at right angles to it; the pair would feel a net 0.71 units. Right, the forces by Ampère's own law of 1826: 0.71 units each, along the line joining the elements, equal and opposite. Both laws give the same force between any two complete circuits, so no experiment on closed circuits can say which is right.

The force between pieces of a current

Ampère spent six years finding the force one short piece of current exerts on another, and the law he found is not the one used today. The modern law, which follows from the Biot–Savart field, disagrees with his for almost every pair of pieces — his obeys Newton's third law and the modern one does not. Both give exactly the same force between any two complete circuits, which is the only thing that has ever been measured. The force between two pieces of current is a quantity with two correct values, because a piece of current on its own does not exist.

5 figures · part 6 on Ampere law
Three shapes of film, one sheet resistance. Three thin films of the same material, of sheet resistance one ohm per square, with four small contacts on each edge labelled A to D in order. For each, the two readings van der Pauw's method takes — the voltage between D and C per unit current from A to B, and between A and D per unit current from B to C — computed by solving for the current flow on a fine grid. For a square, contacts at the corners: 0.221 and 0.221 Ω, giving 1.000 Ω per square; a disc, contacts unevenly spaced: 0.089 and 0.450 Ω, giving 0.999 Ω per square; an irregular lamina: 0.209 and 0.232 Ω, giving 0.999 Ω per square. The readings change with the shape and with where the contacts are; the sheet resistance recovered from them by exp(−πR₁/Rₛ) + exp(−πR₂/Rₛ) = 1 does not.

The sheet resistance that forgets the shape

To measure how well a thin film conducts, the obvious method is to cut it into a neat strip and pass a current along it. In 1958 Leo van der Pauw, an engineer at Philips, showed that the strip is unnecessary. Put four small contacts anywhere on the edge of a film of any shape, take two readings, and one equation returns the film's resistance per square — the shape and the spacing of the contacts drop out entirely. The proof is a single fact about logarithms and the maps that preserve angles, and it fails for exactly one kind of film: one with a hole in it.

5 figures · part 7 on Conductors

Relativity

Space and time, drawn on the same axes.

Sound cones that tip over. Time against position for sound in a fluid that speeds up from 0.55 to 1.3 times the speed of sound, drawn as the cone of places a sound made at each point can reach: its edges move at v − c and v + c. Upstream, where the flow is slow, the cones straddle the vertical and sound can go either way. At x = 0.20, where the flow reaches the speed of sound, the upstream edge stands vertical. Beyond it both edges point downstream: sound made there can no longer reach anywhere upstream of where it was made. That is a horizon, drawn in the same way as the light cones of a black hole, and it arises from nothing but the ordinary addition of a sound's speed to the speed of the water that carries it.

The river that sound cannot swim up

Sound travels at a fixed speed through the air or water carrying it, so a flowing medium adds its own speed to the sound's: faster downstream, slower upstream. That is the plainest velocity addition there is. Where the flow speeds up past the speed of sound, upstream-going sound is carried backwards, and nothing made beyond that point can be heard before it. The point is a horizon. Sound cones tip over there exactly as light cones do at a black hole, and the rate at which the flow speeds up plays the part of the surface gravity. A kitchen sink under a running tap makes the reverse kind of horizon, a white hole for ripples.

5 figures · part 6 on Velocity-addition
An orbit that flattens without being told to. The path of a classical electron relative to its nucleus, in the laboratory, before and after the nucleus has been accelerated gently — over 200 orbits — from rest to 0.6 of the speed of light along the horizontal, computed from Maxwell's field of a moving charge and the relativistic law of motion alone. Before, the orbit is a circle of radius 1. After, it is an ellipse 0.810 wide along the motion and 1.012 across it, a ratio of 0.8003 against 1/γ = 0.8000, and one turn takes 1.2504 times as long as before, against γ = 1.2500. Nothing in the calculation assumed a contraction or a slowing clock: the forces between the moving charges produced both.

The contraction the forces work out for themselves

Relativity usually introduces length contraction as a consequence of how moving observers disagree about simultaneity, not as something that happens to matter. There is a second way to reach the same number, and it is worth knowing because it is the way the idea was first found. Take an atom, accelerate its nucleus gently, and compute what the electron does using only Maxwell's field of a moving charge and the law of motion. Nobody tells the orbit to contract, and it does, by exactly 1/γ, while each turn takes exactly γ times as long. The forces holding matter together work out the contraction for themselves.

5 figures · part 6 on Length contraction
Heat that arrives everywhere at once, and heat that waits. The temperature spread from a point of heat released at time zero, in one dimension, at times 0.5, 2, 8 relaxation times, from the diffusion equation (dashed) and from Cattaneo's telegraph equation (solid) with the same diffusivity, distances in units of the signal speed times the relaxation time. At 0.5, the diffusion equation has put 62 per cent of the heat beyond the reach of any signal; the telegraph equation none, and 78 per cent is still in the two fronts; at 2, the diffusion equation has put 32 per cent of the heat beyond the reach of any signal; the telegraph equation none, and 37 per cent is still in the two fronts; at 8, the diffusion equation has put 5 per cent of the heat beyond the reach of any signal; the telegraph equation none, and 1.8 per cent is still in the two fronts. The fronts, drawn as the vertical marks, carry heat outward at the signal speed and decay; behind them the telegraph solution fills in and, after many relaxation times, becomes the diffusion equation's Gaussian.

The heat that arrives before it could

Release a pulse of heat at one point, and the diffusion equation — the law that has described heat flow since Fourier — says the temperature rises everywhere at once, however far away. A thermometer a kilometre off registers a change the instant the heat is released. That is an infinite signal speed, and relativity forbids it. The flaw is harmless for a kettle and fatal for a relativistic fluid. The repair is a relaxation time: heat flow takes a moment to respond to a temperature gradient. With it the equation carries heat at a finite speed, sends a sharp front ahead of the spreading warmth, and turns short-wavelength heat into a damped wave.

5 figures · part 6 on Relativistic thermodynamics

Quantum

Where the continuous picture runs out, and what replaces it.

A barrier the metal was supposed to choose. The barrier height at a metal contact on n-type silicon against the metal's work function, from Bardeen's model with interface-state densities of none, 10¹² per cm² per eV, 10¹³ per cm² per eV, 10¹⁴ per cm² per eV, a 0.5 nm gap and a neutrality level a third of the gap above the valence band. With no interface states the barrier is Schottky and Mott's φₘ − χ, rising one for one with the work function: from aluminium to platinum, 0.23 to 1.60 eV. With 10¹² per cm² per eV the slope is 0.92 and the same metals give 0.27 to 1.53 eV; with 10¹³ per cm² per eV the slope is 0.53 and the same metals give 0.48 to 1.20 eV; with 10¹⁴ per cm² per eV the slope is 0.10 and the same metals give 0.71 to 0.84 eV. Dense enough interface states pin every barrier near 0.76 eV, and the metal hardly matters.

The barrier the metal cannot choose

Put a metal on a semiconductor and a barrier forms at the interface. The obvious theory says its height is the difference between the metal's work function and the semiconductor's electron affinity. Platinum and aluminium differ by nearly an electronvolt and a half in work function, so they should make wildly different contacts. On silicon and gallium arsenide they do not: nearly every metal gives nearly the same barrier. Bardeen explained why in 1947. A thin layer of electronic states at the interface screens the metal, and it takes only a few such states per hundred surface atoms to pin the barrier wherever they put it.

5 figures · part 5 on Bands
A sharp angle costs a spread of turning. Left: the probability of finding a rotor at each angle, for three states. Right: the probability of each value of its angular momentum, in units of ħ, for the same states. A state bunched to a circular spread of 0.025 has an angular-momentum spread of 2.21ħ; a state bunched to a circular spread of 0.302 has an angular-momentum spread of 0.59ħ; a state with no preferred angle has an angular-momentum spread of 0.00ħ. The angular momentum can only take whole-number values, so its probabilities are bars; the angle is continuous. The state with no preferred angle has exactly one value of angular momentum, and its angle is spread evenly round the circle — where the naive rule would say that its angle's spread times ħ/2 should be infinite, it is π/√3.

The angle the uncertainty principle cannot be written for

Position and momentum trade exactly: squeeze one and the other spreads, with a product never below ħ/2. Angle and angular momentum look like the same pair and are not. A rotor in a state of definite angular momentum has zero spread in angular momentum and a finite spread in angle, π/√3, and their product is zero. Nothing is wrong with the rotor. The relation was written with a commutator that does not hold, because an angle lives on a circle and a line has no ends to wrap round. The relation that does hold measures the angle's spread by how far its average position on the circle falls short of the rim.

5 figures · part 5 on Uncertainty
A pointer that ends up where no eigenvalue could put it. The distribution of a measuring pointer's position, in units of its own initial spread, after it has been coupled to a spin whose two values would move it by ±g. Strongly coupled, g = 3, the pointer splits into two separate spots at ±3: an ordinary measurement. Weakly coupled, g = 0.1, the two possible shifts overlap almost entirely and the pointer's centre moves by only 0.020, the average of the spin times g. Keeping only the 0.99 per cent of runs in which the spin is afterwards found pointing along x, the kept pointer is centred at 0.802 — 8.0 times g, far outside the range ±g that either value of the spin could produce, and approaching the weak value 10, which it would reach exactly for a still weaker coupling.

The value a gentle measurement returns

Couple a pointer to a spin so weakly that the pointer's shift is far smaller than its own blur, and a single run learns almost nothing about the spin. Now keep only the runs in which the spin is later found in a chosen, nearly opposite state. The kept pointers move as though the spin's value were ten, or a hundred, though it can only be plus or minus one. That weak value was predicted in 1988 and has been measured many times. It is not a hidden value of the spin, and it does not break the uncertainty principle: it is paid for exactly in discarded runs. What it does give is a way to watch a quantum system without disturbing it.

5 figures · part 5 on Measurement

Fluids

Matter that will not hold a shape, and the forces that act in it anyway.

Astrophysics

Gravity read as geometry, and the laws carried where no laboratory can follow.

A delay the Planck scale would write into a burst. The arrival delay, relative to a low-energy photon emitted at the same moment, of photons of each energy from a gamma-ray burst at redshift 0.903, if light slowed in proportion to its energy over an energy scale, on logarithmic axes, for that scale at the Planck energy and at ten times and a tenth of it. At the Planck energy a 31 GeV photon would arrive 1.16 s late. The 31 GeV photon from GRB 090510 arrived 0.83 s after the burst began (marked), so a delay of more than that is excluded, and with it any scale below 1.4 times the Planck energy on this simple reading. Fermi's own analysis, allowing for when in the burst the photon could have been emitted, set the limit at 1.2 times the Planck energy: a speed that depends on energy at first order has been excluded at the scale where it was expected.

The photons that raced for seven billion years

Nothing on a laboratory bench can reach the Planck scale, but a gamma-ray burst halfway across the universe can amplify a Planck-scale effect until it is a second long. If spacetime has structure at the Planck length, the simplest guess is that light's speed depends slightly on its energy. Then a burst's high-energy photons would arrive measurably later than its low-energy ones, after a race lasting billions of years. In 2009 a 31 GeV photon from a burst 7.5 thousand million light-years away arrived within 0.83 s of the burst's start. That excludes the simplest version of the idea at the Planck energy itself.

5 figures · part 5 on Planck scale
The strain a lumpy spinning star sends. The gravitational-wave strain at Earth from a neutron star one kiloparsec away, against the wave's frequency — twice the spin frequency — on logarithmic axes, for ellipticities of 10⁻⁹, 10⁻⁷, 10⁻⁵, 10⁻³, with the most each of three known pulsars could emit if all its observed spin-down were gravitational radiation. Crab: at most 1.4·10⁻²⁴ at 59.2 Hz, needing an ellipticity of 7.7·10⁻⁴; Vela: at most 3.3·10⁻²⁴ at 22.4 Hz, needing an ellipticity of 0.0018; J0437−4715: at most 1.6·10⁻²⁶ at 347.4 Hz, needing an ellipticity of 2·10⁻⁸. Searches have pushed the Crab's strain below about a hundredth of its limit, 1.4·10⁻²⁶. The strain grows as the square of the frequency, so a fast millisecond pulsar with a tiny mountain can send as much as a young pulsar with a large one.

The mountain a spinning star is allowed

A neutron star spinning thirty times a second with a bump on its surface a few centimetres high is a rotating mass quadrupole. It sends out gravitational waves at twice its spin frequency, as a steady tone lasting millions of years. None has been heard. The silence is a measurement. The Crab pulsar is slowing down, and if all the energy it loses went into gravitational waves they would have been detected many times over. Searches now say the waves carry less than a ten-thousandth of it. The mountain on the Crab is less than about ten centimetres high, on a star twenty-four kilometres across.

5 figures · part 6 on Gravitational waves
The slice through a mass that a ruler has to climb. A plane through the centre of a uniform body whose compactness 2GM/Rc² is 0.34 — about a neutron star's — drawn as a curved surface on which distances along the surface are the distances rulers measure. The body's edge is a circle whose circumference is 2πR; a ruler laid from the centre to that edge along the surface measures 1.068 R, 6.8 per cent more. Outside the body the surface is Flamm's paraboloid; inside it is a cap of a sphere. The flat line beneath is what Euclid would give. The height of the surface means nothing; only lengths along it are measured. For the Earth the same excess is 1.5 mm in 6,371 km and the surface would be indistinguishable from the flat line.

The radius a mass adds that no circumference shows

Walk round the Earth's equator and divide by 2π, and the number is the Earth's radius. Dig to the centre and measure the same radius with a tape, and the tape comes out about two millimetres longer. Nothing is wrong with either measurement. A mass does not only slow the clocks near it; it stretches the rulers too, and the stretch is exactly as large as the slowing. Clocks cannot see it. Light can, and half of every bend and every delay that light suffers near the Sun is this.

5 figures · part 5 on Gravitational redshift
Two pulls that should be equal and opposite. Two bodies of equal passive mass, one of an ordinary material and one of a material whose active mass is 30 per cent larger than its passive mass (the difference exaggerated to be seen). Each pulls the other with its active mass and is pulled on its passive mass. The pull the unusual body exerts is therefore larger than the pull it receives, the two arrows are not equal and opposite, and the pair, with nothing outside it, accelerates towards the ordinary body. Newton's third law and the conservation of momentum both require the ratio of active to passive mass to be the same for every material, and that is a separate claim from the one torsion balances test, that passive and inertial mass agree.

The pull that has to equal the pull back

Every test of the equivalence principle drops two things and asks whether gravity pulls them equally. None of them asks whether they pull equally. A body's mass enters gravity twice — once as what is pulled and once as what does the pulling — and if the two ratios differed from one material to another, Newton's third law would fail and a lopsided body could push itself through space. The first test of this used a plastic cylinder floating in a liquid. The best uses the Moon, whose light crust is thicker on the side that never faces the Earth.

5 figures · part 6 on Equivalence principle
The heaviest star free neutrons can hold up. Mass against radius for cold stars of free neutrons, each point a different central density, held up by the pressure of the neutrons' exclusion alone: in general relativity and, with the same gas, in Newton's gravity. Relativity's curve reaches a highest mass of 0.71 solar masses at a radius of 9.5 km and turns back; Newton's keeps rising towards 5.8 solar masses as the stars shrink. The measured masses of neutron stars reach about 2.08 (dashed), three times what free neutrons allow, so the matter inside has to be stiffer than a gas of free neutrons: the repulsion between nucleons at short range is holding them up.

The pressure that weighs down what it holds up

In Newton's gravity a star is held up by pressure, and stiffer matter can hold up more: a star of free neutrons could reach almost six solar masses. In general relativity the pressure itself has weight. Every layer squeezed harder to hold up the layers above adds to the pull it is resisting, and past a point pressing harder makes things worse. The same gas of neutrons then tops out at 0.71 solar masses. Neutron stars twice as heavy exist, which says what their insides must be like — and no matter of any kind can hold a static body smaller than nine-eighths of its Schwarzschild radius.

5 figures · part 7 on Self-gravity

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