Part D · Minkowski · spine
Homogeneity, isotropy and the group axioms leave one free constant, a speed; fix it, and every paradox of special relativity becomes a statement about one indefinite bilinear form.
needs 03, 14~2½ h slides + 5 h problemsproblems: ./mr problems 26
26 · overview
One twin stays on Earth. The other flies at $0.8c$ to a star $4$ light-years away and straight back. Earth's clock reads $10$ years at the reunion; the traveller's reads $6$. Each thinks the other's clock runs slow, so why is the traveller the younger?
1 Integrate proper time along each worldline: $10$ and $6$. 2 Count the one-a-year radio signals each twin receives: $10$ and $6$, and see when the Doppler shift flips. 3 Draw the traveller's lines of simultaneity on a correctly scaled diagram and watch them jump $6.4$ years at the turn.
Answer 1 is a theorem about the quadratic form $-c^2t^2 + x^2 + y^2 + z^2$, where time enters with the opposite sign to space: for it, the straight path between two events is the longest, not the shortest. The twin paradox is the reversed triangle inequality.
A dotted underline is a glossary term: click it, or press G. N opens the notes, where the longer proofs live. A solid underline, like the twins, shows the running example on hover.
section 1
Which changes of inertial frame are possible at all — before anyone mentions light.
26 · the group
An event is a point of spacetime: a place at an instant. An inertial frame is a coordinate system $(t, x, y, z)$ on the set of events in which every free particle moves on a straight line at constant speed. A worldline is the set of events a particle occupies.
No experiment distinguishes one inertial frame from another. So the coordinate changes between inertial frames form a group $G$, and the change to a frame moving at velocity $\vec v$ depends on $\vec v$ alone.
The question. What can $G$ be? Unit 03 answered, without saying so, with the Galilean boost $t' = t$, $x' = x - vt$. Unit 25 showed that Maxwell's equations are not invariant under it. So assume less, and see what is forced.
homogeneity: no event is special. isotropy: no spatial direction is special. group: frame changes compose and invert, depend continuously on $\vec v$, and $\vec v = 0$ is the identity.
Einstein's second postulate — the speed of light is independent of its source — is not among them. It will be needed for exactly one thing.
26 · the group
Let $f: \mathbb R^4 \to \mathbb R^4$ send an event's $S$-coordinates to its $S'$-coordinates. Homogeneity: the $S'$-separation of two events depends only on their $S$-separation, $$f(X + A) - f(X) = g(A)\quad\text{for all } X, A.$$
If $f$ is continuous and homogeneous, then $f(X) = f(0) + \Lambda X$ with $\Lambda$ linear.
$g(A + B) = f(X + A + B) - f(X + A) + f(X + A) - f(X) = g(B) + g(A)$: $g$ is additive. Additive gives $g(qA) = q\,g(A)$ for rational $q$, and continuity extends it to real $q$. So $g$ is linear, and $f(X) = f(0) + g(X)$.
Choose the origins so the two frames' spatial origins coincide at $t = t' = 0$; then $f(0) = 0$ and $f = \Lambda$ is a $4\times 4$ matrix. Physically: straight worldlines go to straight worldlines, as they must if both frames are inertial.
26 · the group
Rotate both frames' axes so $\vec v = v\,\hat x$. Isotropy then forces the transverse coordinates to be left alone:
$$y' = y,\qquad z' = z,$$and the $(t, x)$ block to decouple from them. What remains is a $2\times 2$ matrix $L(v)$ acting on $(t, x)$.
The origin of $S'$ moves along $x = vt$, and $x' = 0$ there, so the second row is fixed up to a factor:
$$x' = \gamma(v)\,(x - vt),\qquad t' = a(v)\,t + b(v)\,x.$$Mirror. Reflecting $x \mapsto -x$ in both frames turns a boost by $v$ into a boost by $-v$: $L(-v) = PL(v)P$, $P = \operatorname{diag}(1, -1)$. So $a$ and $\gamma$ are even in $v$, and $b$ is odd.
Reciprocity. $L(v)^{-1} = L(-v)$: if $S'$ moves at $v$ in $S$, then $S$ moves at $-v$ in $S'$. This one needs a proof, in the notes; it forces $a = \gamma$.
26 · the group
Under homogeneity, isotropy and the group axioms, there is a constant $K$, the same for every $v$, with
$$t' = \gamma\,(t - Kvx),\qquad x' = \gamma\,(x - vt),\qquad \gamma = \frac{1}{\sqrt{1 - Kv^2}}.$$With $a = \gamma$ and $K(v) := -b/(\gamma v)$, $L(v) = \gamma\left(\begin{smallmatrix}1 & -Kv\\ -v & 1\end{smallmatrix}\right)$. Reciprocity, $L(v)^{-1} = L(-v)$, forces $\det L(v) = \gamma^2(1 - Kv^2) = 1$. The product $L(v)L(u)$ has diagonal entries $\gamma_v\gamma_u(1 + K(v)vu)$ and $\gamma_v\gamma_u(1 + K(u)uv)$; it is a boost, so they are equal, and $K(v) = K(u)$.
Check. $[Kvx] = [t]$ needs $[K] = \mathrm{s^2\,m^{-2}}$: $K^{-1/2}$ is a speed ✓. $v \to 0$: $\gamma \to 1$, identity ✓.
The structure leaves exactly one number undetermined. $K > 0$ gives the Lorentz transformation, with $c := K^{-1/2}$; the sign of $K$ decides which world we are in — drawn on the next slide.
26 · the group
Where a moving clock's first tick, $t' = 1$, lands in $S$ for several $v$ (dots, each on that frame's time axis $x = vt$). The boosts slide it along the curve $t^2 - Kx^2 = 1$: a line, a hyperbola inside the light lines, or a circle — and only on the circle can composing boosts carry it to $t < 0$ (dashed).
$K = 0$: Galileo, $t' = t$, $x' = x - vt$. $K > 0$: Lorentz, $c = K^{-1/2}$. $K < 0$: rotations of the $(t, x)$ plane — two boosts can turn a clock's time backwards. Excluded.
Why the curve. In $S$ the tick is at $(x, t) = (\gamma v, \gamma)$, by the inverse boost at $x' = 0$, $t' = 1$. So $t^2 - Kx^2 = \gamma^2(1 - Kv^2) = 1$ for every $v$: one curve per world.
26 · the group
For $K = 1/c^2$ the composite velocity is $w = \dfrac{u + v}{1 + uv/c^2}$. Put $u = c$: $w = c$ for every $v$. Something moving at $c$ in one frame moves at $c$ in all of them. Proof: one line of algebra.
| postulate | what it does here |
|---|---|
| relativity | makes the frame changes a group, gives reciprocity via isotropy, makes $K$ a constant |
| light speed independent of source | chooses $K > 0$ over $K = 0$, and names the invariant speed: light's |
Unit 25 earned the value: the wave operator $\partial_t^2/c^2 - \nabla^2$ of Maxwell's theory is invariant under exactly this group with this $c$. If you have not done unit 25, you are taking $K = 1/c^2$ on credit here, with $c = 299\,792\,458\ \mathrm{m\,s^{-1}}$ (exact, by the definition of the metre).
$c = 1$, $v = 0.8$, $\gamma = 5/3$. $T = (t, x) = (5, 4)$: $t' = \tfrac53(5 - 0.8\cdot 4) = 3$, $x' = \tfrac53(4 - 0.8\cdot 5) = 0$. At the traveller's own position, after three years ✓.
section 2
What the Lorentz transformations preserve, and everything that follows from asking only that.
26 · the form
With $x^0 = ct$, every Lorentz transformation preserves the interval
$$s^2 = -(x^0)^2 + x^2 + y^2 + z^2 .$$$x^{0\prime} = \gamma(x^0 - \beta x)$, $x' = \gamma(x - \beta x^0)$ with $\beta = v/c$. Then $x'^2 - x^{0\prime 2} = \gamma^2(1 - \beta^2)(x^2 - x^{0\,2}) = x^2 - x^{0\,2}$, and $y, z$ are untouched.
So the physics — the group — has an invariant, and it is a quadratic form. Turn the logic round and define the setting by the form:
Spacetime is a 4-dimensional real vector space with a symmetric bilinear form of a certain signature. The Lorentz group is the group of that form. Every kinematic effect is a property of the form.
Check. $s^2$ is a length squared in every term ✓. On the turn: $-25 + 16 = -9$ in $S$ and $-9 + 0 = -9$ in $S'$ ✓.
26 · the form
A 4-dimensional real vector space $V$ with a symmetric bilinear form $\eta: V\times V\to\mathbb R$ of signature $(-,+,+,+)$: some basis $(e_0, e_1, e_2, e_3)$ has $\eta(e_\mu, e_\nu) = \eta_{\mu\nu}$, $\eta_{\mu\nu} = \operatorname{diag}(-1, 1, 1, 1)$. Such a basis is a Lorentz orthonormal basis: an inertial frame.
The Minkowski form $\eta$ is the object; its matrix is what it looks like in one basis. Events form an affine space over $V$; differences of events are vectors.
For $X = X^\mu e_\mu$, $Y = Y^\nu e_\nu$: $\ \eta(X, Y) = \eta_{\mu\nu}X^\mu Y^\nu$, a repeated upper-lower index summed over $0..3$. Notation, nothing more.
If $e'_\alpha = \Lambda^\mu{}_\alpha\, e_\mu$ is another basis, then $\eta'_{\alpha\beta} = \Lambda^\mu{}_\alpha\Lambda^\nu{}_\beta\,\eta_{\mu\nu}$, i.e. $\eta' = \Lambda^{\mathsf T}\eta\Lambda$.
Proof: $\eta'_{\alpha\beta} = \eta(e'_\alpha, e'_\beta) = \eta(\Lambda^\mu{}_\alpha e_\mu, \Lambda^\nu{}_\beta e_\nu)$; expand by bilinearity.
26 · the form
timelike if $\eta(X,X) < 0$; null if $\eta(X,X) = 0$; spacelike if $\eta(X,X) > 0$. The null vectors form the light cone. A timelike or null $X$ is future-directed if $X^0 > 0$.
Because $\eta$ is invariant, the classification is the same in every inertial frame: it is a property of the pair of events, not of the observer.
Out-leg $X = (5, 4)$: $-25 + 16 = -9$, timelike. A light ray $(4, 4)$: null. The separation from Earth-at-$t{=}5$ to $T$, $(0, 4)$: $+16$, spacelike.
The plane $(x, x^0)$, years and light-years. The cone $x^0 = \pm x$ splits it; each of the twins' three vectors, components $(x^0, x)$, ends where its $\eta(X, X)$ puts it.
26 · the form
If $X, Y$ are future-directed timelike, $\eta(X, Y) < 0$. Proof: $\eta(X,Y) = -X^0Y^0 + \vec x\cdot\vec y \le -X^0Y^0 + |\vec x||\vec y| < 0$, by Cauchy–Schwarz in $\mathbb R^3$ and $|\vec x| < X^0$, $|\vec y| < Y^0$.
In the picture: the vectors $\eta$-orthogonal to $X$ form the line $X^\perp$, the mirror image of $X$ in the light line. It lies outside the cone, so it is spacelike, and the whole future cone sits on its negative side.
In $(+,-,-,-)$ every inequality above flips: timelike means $\eta(X,X) > 0$. Check which convention a book uses before copying a formula.
$X$ and $Y$ are the twins' two legs, components $(x^0, x)$; $\eta(X, Y) = -25 - 16 = -41$. $Z = (4, 5)$ has $\eta(X, Z) = -20 + 20 = 0$: the line $X^\perp$ (dashed) is spacelike, and every future timelike vector is on the side where $\eta(X, \cdot) < 0$.
26 · the form
$\{\Lambda \in GL(V) : \eta(\Lambda X, \Lambda Y) = \eta(X, Y)\ \forall X, Y\}$. In an orthonormal basis: $\Lambda^{\mathsf T}\eta\Lambda = \eta$.
Two continuous invariants: $\det\Lambda = \pm1$ (take determinants: $\det(\Lambda)^2 = 1$), and whether $\Lambda$ maps the future cone to itself, which happens iff $\Lambda^0{}_0 \ge 1$; otherwise $\Lambda^0{}_0 \le -1$.
| $\Lambda^0{}_0 \ge 1$ | $\Lambda^0{}_0 \le -1$ | |
|---|---|---|
| $\det = +1$ | $SO^+(1,3)$: boosts, rotations | $PT$ |
| $\det = -1$ | $P = \operatorname{diag}(1,-1,-1,-1)$ | $T = \operatorname{diag}(-1,1,1,1)$ |
$O(1,3)$ has exactly four connected components, the cells of the table. The identity's component, the proper orthochronous group $SO^+(1,3)$, is a normal subgroup; the others are its cosets $P\,SO^+$, $T\,SO^+$, $PT\,SO^+$.
26 · the form
For $|\beta| < 1$ put $\varphi = \operatorname{artanh}\beta$. Then $\gamma = \cosh\varphi$, $\gamma\beta = \sinh\varphi$, and
$$B(\varphi) = \begin{pmatrix}\cosh\varphi & -\sinh\varphi\\ -\sinh\varphi & \cosh\varphi\end{pmatrix}.$$$B(\varphi)B(\psi) = B(\varphi + \psi)$. The boosts along one axis form a one-parameter group isomorphic to $(\mathbb R, +)$.
Proof: multiply, and use $\cosh(\varphi+\psi) = \cosh\varphi\cosh\psi + \sinh\varphi\sinh\psi$ and its partner for $\sinh$.
A boost slides points along the hyperbolae $x^2 - (x^0)^2 = $ const, as a rotation slides them along circles (arrows: $B(\varphi)$, $\varphi > 0$). Dots: $e_0$ moved by $\varphi = 0, \pm0.5, \pm1$. The light lines are only rescaled.
26 · the form
Since $|\tanh| < 1$ on $\mathbb R$, composing boosts can never reach $c$.
Rapidities add; speeds are their $\tanh$. Equal boosts are equal steps along the $\varphi$ axis, and $\tanh$ squashes the steps ever closer below $1$.
Check. $\beta_u = 1$: $\beta_w = (1 + \beta_v)/(1 + \beta_v) = 1$, the invariant speed ✓.
Repeated boosts of $0.5c$, each adding $\tfrac12\ln 3 = 0.549$ to $\varphi$: $\beta = 0.5, 0.8, 0.929, 0.976, 0.992$ (dots, $\beta = \tanh\varphi$). Galileo's sum (dashed) reaches $c$ after two.
26 · the form · example
1. $\varphi_{1/2} = \operatorname{artanh} 0.5 = \tfrac12\ln\dfrac{1 + 0.5}{1 - 0.5} = \tfrac12\ln 3 = 0.5493$.
2. Two such boosts: $\varphi = \ln 3 = 1.0986$.
3. $\beta = \tanh(\ln 3) = \dfrac{3 - 1/3}{3 + 1/3} = \dfrac{8}{10} = 0.8$.
4. Direct check: $\dfrac{0.5 + 0.5}{1 + 0.25} = 0.8$ ✓. And $\gamma = \cosh\ln 3 = \tfrac12(3 + \tfrac13) = \tfrac53$ ✓.
The traveller's rapidity is $\ln 3$, so $e^{\varphi} = 3$. Section 3 shows that $e^{\varphi}$ is the Doppler factor: that is why the signal counts come in threes.
Galileo would say two $0.5c$ boosts make $1.0c$. Rapidity says each successive $0.5c$ boost adds the same $0.549$ to $\varphi$, and $\beta = \tanh\varphi$ creeps towards $1$ without reaching it. The problems page does ten of them.
26 · the form
Write $p \prec q$ if $q - p$ is a nonzero future-directed timelike or null vector. Let $f:\mathbb R^4\to\mathbb R^4$ be any bijection with $p \prec q \iff f(p) \prec f(q)$. Then $f$ is a composition of an orthochronous Lorentz transformation, a translation and a dilation $X \mapsto \lambda X$, $\lambda > 0$.
Zeeman, "Causality implies the Lorentz group", J. Math. Phys. 5 (1964) 490–493; Alexandrov proved the version for light-cone-preserving maps in the 1950s.
What it removes. No linearity, no continuity, no homogeneity: section 1's lemma is not needed. Preserving "could have caused" is already enough to force the group, up to the scale of the units.
In one space and one time dimension it is false: with $u = x^0 + x$, $w = x^0 - x$, any $(u, w)\mapsto(F(u), H(w))$ with $F, H$ increasing bijections preserves $\prec$. A problem on the sheet.
section 3
The actual content of special relativity; dilation and contraction are corollaries.
26 · simultaneity
Two events with $\Delta t = 0$ and $\Delta x \ne 0$ in $S$ have, in $S'$,
$$\Delta t' = -\gamma\,\frac{v\,\Delta x}{c^2} \ne 0 .$$In $S'$, the event further along $+x$ happens first.
The lines of constant $t'$ are $t - vx/c^2 = \text{const}$: in an $(x, ct)$ diagram they tilt up with slope $\beta$. They are exactly the vectors $\eta$-orthogonal to the observer's worldline.
$\beta = 0.5$, $c = 1$. $A$ and $B$ share $S$'s horizontal "now". $B$ is on the $x'$ axis, $t' = 0$; the line of constant $t'$ through $A$ (dashed) meets the $ct'$ axis at $t' = \gamma = 1.15$. So $\Delta t'_{B-A} = -\gamma v\Delta x/c^2 = -1.15$.
26 · simultaneity
A clock at rest sends light at $t_1$ to a distant event $E$, and gets the reflection back at $t_2$. It defines $E$ to have happened at $t_E = \tfrac12(t_1 + t_2)$, at distance $\tfrac12 c(t_2 - t_1)$.
Apply that definition in each frame and you get each frame's own simultaneity, and they differ. No experiment picks one: the choice is a convention, and the group says all choices are equally good.
For a moving observer, the radar "now" is the tilted line of the previous slide: light out and back at $45°$ makes the triangle symmetric about it.
An observer at $\beta = 0.5$ times the echo from $E$: out at $\tau_1$, back at $\tau_2$, so $E$ is assigned the clock reading $\tfrac12(\tau_1 + \tau_2)$. That event and $E$ lie on a line of slope $\beta$ — the observer's now — not on $S$'s horizontal one.
26 · simultaneity
A clock at rest in $S'$ ticks at $\Delta x' = 0$. By the inverse boost, $\Delta t = \gamma(\Delta t' + v\Delta x'/c^2) = \gamma\,\Delta t'$: the moving clock's ticks are $\gamma$ times further apart in $S$.
Muons in the CERN storage ring at $\gamma = 29.3$: rest lifetime $2.197\ \mu$s, so $\gamma\tau = 64.4\ \mu$s predicted and seen to about $0.1\%$ (Bailey et al., Nature 268, 1977).
A rod at rest in $S'$ has ends at $x' = 0$ and $x' = L_0$. Its length in $S$ is the separation of its ends at one $S$-instant. $x' = \gamma(x - vt)$ at fixed $t$ gives $\Delta x = L_0/\gamma$.
Both follow in one line from the boost. What they mean is clearer drawn, once diagrams are drawn honestly: "Length contraction is a slice of a strip", two slides on, cuts a rod's history two ways.
26 · simultaneity
$\beta = 0.6$. Primed axes (thick) and the calibration hyperbolae $-(x^0)^2 + x^2 = \mp1$ (curves), which cross each axis at its unit tick: the primed ticks $1'$ sit further out on paper than the unprimed $1$.
The $ct'$ axis is the worldline $x = \beta\,ct$; the $x'$ axis is the simultaneity line $ct = \beta x$. Both lean towards the light line by the same angle.
The paper is Euclidean; the form is not. The unit tick on the $ct'$ axis is at $(x, ct) = (\gamma\beta, \gamma)$, a Euclidean distance $\sqrt{(1+\beta^2)/(1-\beta^2)}$ from the origin: $1.46$ at $\beta = 0.6$, $2.13$ at $\beta = 0.8$. Find it where the hyperbola crosses, not with a ruler.
26 · simultaneity
A rod of rest length $L_0 = 2$ moving at $\beta = 0.6$ ($\gamma = 1.25$), $c = 1$. Its history is the shaded strip. $S$'s "now" cuts it in $L_0/\gamma = 1.6$; the rod's own "now", of slope $\beta$, cuts it in a segment whose end lies on the calibration hyperbola $x^2 - (ct)^2 = 4$: proper length $2$.
Dilation compares one clock with two of the other frame's, which must be synchronised; contraction measures two ends at one instant. Change the simultaneity and both change. Neither is a mechanism acting on clocks or rods.
There is one rod and one strip. "Its length" is the length of a slice, and which slice depends on whose "now" you cut with. Neither slice is the rod's true length; $L_0$ is the one cut by the rod's own simultaneity.
26 · simultaneity · example
Earth frame, years and light-years. Red dashed: the traveller's simultaneity through $T$, before and after the turn; grey: the same at each traveller year, meeting Earth at $0.6$-year steps.
1. Outbound simultaneity through $T = (5, 4)$ has slope $\beta = 0.8$: $t - 5 = 0.8(x - 4)$. At $x = 0$: $t = 5 - 3.2 = 1.8$.
2. Inbound, $\beta = -0.8$: $t - 5 = -0.8(x - 4)$. At $x = 0$: $t = 5 + 3.2 = 8.2$.
3. Outbound, the traveller's "Earth now" advances from $0$ to $1.8$ in $3$ years of the traveller's clock: rate $0.6 = 1/\gamma$, dilation ✓. Inbound, $8.2 \to 10$ in $3$ years: again $0.6$.
4. At the turn it jumps from $1.8$ to $8.2$: $6.4$ years. Total $1.8 + 6.4 + 1.8 = 10$ ✓.
26 · simultaneity
A pole $20$ m long (rest length) runs at $\gamma = 2$ into a barn $10$ m long with a door at each end. In the barn's frame the pole is $10$ m: both doors can be shut at once with the pole inside. In the pole's frame the barn is $5$ m: the pole can never be inside. Which is it?
Both pictures are correct contraction arithmetic. The trouble is the word "inside", which means "inside at one instant" — and the two frames do not share instants.
The two frames' pictures, to one scale. Each is right about lengths; each "now" is a different set of events.
26 · simultaneity
Barn frame, metres. Both door events (dots) lie on the barn's now, $ct = 0$, with the pole's strip between them. The pole's now through the back-door event (dashed, slope $\beta = 0.866$) meets the front door $8.66$ m of light-time before it shuts.
"Both doors shut at once" is a statement about two events $10$ m apart with $\Delta t = 0$ — a spacelike pair. In the pole's frame they are not simultaneous: the back door shuts first, by $\gamma\beta\cdot10\ \mathrm{m}/c = 57.8$ ns.
No contradiction: the frames disagree about when, and "the pole is inside" means "inside at one instant". Nothing frame-independent — a collision, a broken pole — differs. The problems page writes the events out and transforms them.
26 · simultaneity
A source recedes at $\beta$ and emits pulses a proper time $T_0$ apart. The receiver's pulses are $T$ apart, with
$$\frac{T}{T_0} = \sqrt{\frac{1+\beta}{1-\beta}} = e^{\varphi}.$$Approaching: $e^{-\varphi}$. Frequencies go the other way.
Proof. Receiver at the origin; source on $x = vt$, emitting at $t = 0$ and $t = \gamma T_0$. The second pulse starts $v\gamma T_0$ further away, so arrives $\gamma T_0(1 + \beta)$ after the first. $\gamma(1+\beta) = \sqrt{(1+\beta)/(1-\beta)}$.
Check. $\beta\to0$: $e^\varphi \approx 1 + \beta$, the classical Doppler shift ✓. $\beta\to1$: infinite stretch, redshift to nothing ✓.
The proof, drawn for the traveller: $\beta = 0.8$, $T_0 = 1$ yr, $c = 1$. Ticks at $t = \gamma T_0 = 5/3$ and $10/3$; each extra $\beta\gamma T_0$ of distance adds that much light-time. Arrivals at $3$ and $6$: $T = \gamma(1 + \beta)T_0 = 3T_0$.
26 · simultaneity
Relay a signal through a chain of observers each receding from the last: the factors multiply, since $e^{\varphi}e^{\psi} = e^{\varphi+\psi}$. A second proof of velocity addition, needing only light rays.
For the traveller, $e^{\ln 3} = 3$. Outbound, one pulse a year arrives every $3$ years; inbound, every $4$ months.
The factor $e^{\varphi}$ is the one "Boosts are hyperbolic rotations" found on the light lines: a boost stretches one null direction by exactly the Doppler factor.
The traveller's $0.8c$ as two $0.5c$ steps: $B$ recedes from $A$ at $0.5c$, $C$ from $B$ at $0.5c$. Light from $C$'s yearly ticks passes $B$ every $\sqrt3$ years of $B$'s clock and reaches $A$ every $3$: $\sqrt3\cdot\sqrt3 = 3$.
26 · simultaneity · example
Earth sends a pulse each Earth year. Outbound ($3$ yr of the traveller's clock) they arrive $3$ yr apart: $1$ pulse. Inbound ($3$ yr) they arrive every $\tfrac13$ yr: $9$ pulses.
Total $10$: Earth aged $10$ years. The flip comes at the traveller's turn, half-way through the traveller's trip.
The flip is on the traveller's own worldline, at the turn: everything sent after Earth's year $1$ is met on the way back.
Earth frame. Earth's yearly pulses (orange, at $45°$): only year $1$'s reaches the traveller before $T$.
26 · simultaneity · example
The traveller sends a pulse each of the traveller's years. Light from the turn at $(5, 4)$ reaches Earth at $t = 5 + 4 = 9$. For $9$ years, pulses arrive $3$ yr apart: $3$ pulses. In the last year, every $\tfrac13$ yr: $3$ pulses.
Total $6$: the traveller aged $6$ years. The flip comes at year $9$ of $10$.
Both twins see the other's clock slow by $3$ while separating and fast by $3$ while approaching. The traveller spends half the trip in each; Earth spends $9$ years seeing slow and $1$ seeing fast, because it learns of the turn only when its light arrives. No acceleration appears in the count.
Earth frame. The traveller's yearly pulses: three outbound ones reach Earth at years $3$, $6$, $9$; the light of the turn (red) arrives at year $9$; three inbound ones crowd into the last year.
26 · simultaneity
A source moving at $\beta$ along $x$ emits light at angle $\theta'$ to $x$ in its own frame. In the lab the angle is $\theta$ with
$$\cos\theta = \frac{\cos\theta' + \beta}{1 + \beta\cos\theta'}.$$Proof. The ray's direction is a null vector, $(1, \cos\theta', \sin\theta', 0)$ in the source frame. Boost by $-\beta$: $(\gamma(1 + \beta\cos\theta'),\ \gamma(\cos\theta' + \beta),\ \sin\theta',\ 0)$. It is still null, and $\cos\theta$ is its $x$ part over its time part.
Stellar aberration. The Earth's orbital $\beta \approx 29.8/299\,792 = 9.9\times10^{-5}$ shifts starlight by up to $\beta$ radians: $20.5''$, which Bradley measured in 1728.
Check. $\beta = 0$: $\theta = \theta'$ ✓. $\theta' = 0$: $\theta = 0$ ✓.
What the formula does to a whole sky of rays is the headlight effect, drawn on the next slide.
26 · simultaneity
Thirteen rays every $15°$, emitted isotropically in the source frame (left), seen in the lab with the source moving right at $\beta = 0.8$ (right). The forward seven (blue), which filled $90°$, are squeezed into $\theta \le \arccos 0.8 = 36.9°$.
Emission that is isotropic in the source frame puts half its light ($\theta' < 90°$) into the lab cone $\cos\theta > \beta$, i.e. $\sin\theta < 1/\gamma$. At $\gamma = 10$: a cone of half-angle $5.74°$. Synchrotron light is beamed for this reason.
Each ray keeps its order: aberration is a monotone map of $[0°, 180°]$ onto itself. It only redistributes the rays, crowding the forward half into a cone that shrinks like $1/\gamma$.
section 4
Which parts of "before" survive a change of frame, and why nothing outruns light.
26 · causality
(a) If $q - p$ is timelike or null, every orthochronous Lorentz transformation preserves the sign of $\Delta t$.
(b) If $q - p$ is spacelike, there are inertial frames in which $\Delta t' > 0$, $= 0$ and $< 0$.
(a) Orthochronous maps send the future cone to itself (the cone's closure too, by continuity). (b) Align $x$ with $\Delta\vec x$, so $|\Delta x| > c|\Delta t|$. Then $\Delta t' = \gamma(\Delta t - v\Delta x/c^2)$, and $v$ ranges over $(-c, c)$, so $v\Delta x/c^2$ takes every value in $(-|\Delta x|/c,\ |\Delta x|/c) \ni \Delta t$.
$J^+(p) = \{q : q - p \text{ future causal or } 0\}$, and $J^-(p)$ likewise. The elsewhere of $p$ is everything outside $J^+(p)\cup J^-(p)$: events whose order relative to $p$ is a matter of frame.
$q$ is spacelike to $p$. Through $p$, three frames' lines of simultaneity put $q$ after $p$, level with it, or before it. No such line can pass above an event in $J^+(p)$.
26 · causality · example
Earth-at-$t{=}5$ is spacelike to $T$. Outbound frame: $\Delta t' = \tfrac53(0 - 0.8\cdot(-4)) = +5.33$ yr, after $T$. Inbound frame: $\tfrac53(0 + 0.8\cdot(-4)) = -5.33$, before. The elsewhere of $T$ on Earth is $1 < t < 9$ — the Doppler flip times.
The traveller's two frames disagree about the order of $T$ and Earth-at-year-$5$. That is the $6.4$-year jump of "The twins on the diagram", seen as an ordering — and the window's ends are exactly the radio flips.
Earth frame. $J^\pm(T)$ shaded; Earth between years $1$ and $9$ (orange) is $T$'s elsewhere. Earth-at-$5$ is above the outbound "now" through $T$ (to $1.8$) and below the inbound one (to $8.2$).
26 · causality
Suppose signals could be sent at some speed $u > c$, in every inertial frame (relativity). Then some sequence of two such signals arrives at its sender's worldline before it was sent.
Emission $p$ at the origin, reception $q = (\Delta t, u\Delta t)$: spacelike. In the frame with $c^2/u < v < c$, $\Delta t' = \gamma\Delta t(1 - uv/c^2) < 0$: the signal runs backwards in time. The receiver, at rest in that frame, replies with its own speed-$u$ signal backwards to the sender, arriving in the sender's past (details in the notes).
$c = 1$, $u = 2$, Bob at $v = 0.9$. Bob's "now" through $q$ passes below $p$, so for him the question arrives before it is sent. His reply (red), at $u$ in his frame, reaches Alice at $t = -0.45$.
26 · causality
One backwards-in-time signal is odd but not contradictory. The contradiction is the loop: a reply that reaches the sender before the question left, who then does not send it. Relativity plus "no causal loops" forbids signals faster than $c$. Neither alone does.
If $u < c$, then $uv/c^2 < 1$ for every $|v| < c$, so $\Delta t'$ has the sign of $\Delta t$ in every frame — part (a) of the theorem on "What survives of 'before'".
Put together: if relativity holds, and nothing can arrive at its own past to stop itself being sent, then nothing travels faster than $c$. The light cone is the boundary of every possible influence.
section 5
The length of a timelike curve, and the inequality that makes straight lines the longest.
26 · proper time
For a future-directed timelike curve $\lambda\mapsto X(\lambda)$, piecewise $C^1$, $\lambda\in[a, b]$:
$$\tau[X] = \frac1c\int_a^b\sqrt{-\eta_{\mu\nu}\,\dot X^\mu\dot X^\nu}\ \mathrm d\lambda .$$Parametrised by the frame's $t$, with $\vec x(t)$: $\ \tau = \displaystyle\int\sqrt{1 - |\dot{\vec x}|^2/c^2}\ \mathrm dt$.
It is invariant twice over: under reparametrisation (as unit 03's arc length is), and under Lorentz transformations (the integrand is built from $\eta$).
An ideal clock carried along a worldline reads its proper time, whatever its acceleration. The storage-ring muons, at about $10^{18}\,g$, obeyed it.
Check. $[\eta\,\dot X\dot X] = \mathrm m^2$ per unit of $\lambda$ squared, so the integral is a length; over $c$, a time ✓. At rest, $\tau = \Delta t$ ✓. Constant speed, $\tau = \Delta t/\gamma$: time dilation ✓.
26 · proper time · example
Earth. $\vec x(t) = 0$ for $0 \le t \le 10$: $\tau_E = \int_0^{10} 1\,\mathrm dt = 10$ yr.
Traveller, out. $\dot x = 0.8$ on $[0, 5]$: $\int_0^5\sqrt{1 - 0.64}\,\mathrm dt = 5\times0.6 = 3$ yr.
Traveller, back. $\dot x = -0.8$ on $[5, 10]$: again $3$ yr.
Total. $\tau_T = 6$ yr. The traveller is $4$ years younger.
As vectors. Out $X = (5, 4)$, back $Y = (5, -4)$: $\sqrt{25 - 16} = 3$ each. Straight $X + Y = (10, 0)$: $10$.
Earth frame. Dots: one-year ticks of each twin's own clock. Ten on the straight worldline, six on the bent one, though its ticks look further apart on paper ($5/3$ Earth years each).
26 · proper time · example
Replace the instant turn by one lasting Earth-time $\delta$. Its contribution to $\tau_T$ is at most $\delta$, since the integrand is at most $1$. As $\delta\to0$ it vanishes, and the $4$-year difference does not. Acceleration marks which twin's worldline is bent; it is not where the time goes.
The age difference is accumulated during the coasting legs, uniformly, because the bent path is shorter in the sense of $\eta$. The next slide proves that bent is always shorter.
The instant turn replaced by one lasting $\delta = 1$ or $2$ Earth years, speed going linearly from $+0.8c$ to $-0.8c$. The traveller's proper time grows only by $0.28\,\delta$; as $\delta\to0$ it returns to $6$, and the $4$-year gap stays.
26 · proper time
If $X$ is timelike and $Y$ is any vector, $\ \eta(X, Y)^2 \ge \eta(X, X)\,\eta(Y, Y)$, with equality iff $Y$ is a multiple of $X$.
Write $Y = aX + Z$ with $\eta(X, Z) = 0$. $Z$ is $0$ or spacelike (lemma of section 2). Then $\eta(X,Y)^2 = a^2\eta(X,X)^2$ and $\eta(X,X)\eta(Y,Y) = a^2\eta(X,X)^2 + \eta(X,X)\eta(Z,Z)$. The last term is $\le 0$, and $= 0$ iff $Z = 0$.
With $\lVert X\rVert := \sqrt{-\eta(X, X)}$, for future-directed timelike $X, Y$:
$$\lVert X + Y\rVert \ \ge\ \lVert X\rVert + \lVert Y\rVert ,$$with equality iff $X, Y$ are parallel.
$\lVert X + Y\rVert^2 = \lVert X\rVert^2 + \lVert Y\rVert^2 - 2\eta(X, Y)$. By the section 2 lemma $\eta(X, Y) < 0$, and by reversed Cauchy–Schwarz $-\eta(X, Y) \ge \lVert X\rVert\,\lVert Y\rVert$. So the right side is $\ge (\lVert X\rVert + \lVert Y\rVert)^2$.
26 · proper time
Let $q - p$ be future timelike. Among all future-directed timelike piecewise-$C^1$ curves from $p$ to $q$, the straight segment has the greatest proper time, $\lVert q - p\rVert/c$, and it is the only one that does.
Boost and translate so $p = 0$ and $q = (cT, \vec 0)$. Parametrise by $t\in[0, T]$. Then $\tau = \int_0^T\sqrt{1 - |\dot{\vec x}|^2/c^2}\,\mathrm dt \le T$, with equality iff $\dot{\vec x} \equiv 0$.
Zig-zag at speed $\beta c$ between $p$ and $q$: $\tau = T\sqrt{1 - \beta^2} \to 0$ as $\beta \to 1$. The infimum is $0$ and is not attained.
From $p$ to $q$, $10$ years apart on the straight clock. The twins' path at $0.8c$: $6$. A zig-zag at $0.95c$, never more than $1.2$ light-years from the straight line: $3.1$. Faster zig-zags push it towards $0$.
26 · proper time
Unit 11 asked whether a stationary curve is a minimum. For $\tau$ the Lagrangian in $\dot x$ is $F = \sqrt{1 - \dot x^2/c^2}$:
$$F_{\dot x\dot x} = -\frac{1}{c^2\,(1 - \dot x^2/c^2)^{3/2}} < 0 .$$Unit 11's Legendre condition for a minimum, $F_{\dot x\dot x} \ge 0$, fails everywhere; the one for a maximum holds everywhere. The sign of $\eta$ has turned the variational problem upside down.
The two integrands against $\dot x$ ($c = 1$). Arc length's is convex: a zig-zag at $\pm0.8$ averages $1.28 > 1$, so straight is shortest. Proper time's is concave: the zig-zag averages $0.6 < 1$, so straight is longest.
26 · proper time
Unit 32 says free fall follows geodesics, and unit 27 takes $-mc^2\tau$ as the free action. In Lorentzian signature a timelike geodesic is a local maximum of proper time: a freely falling clock ages the most.
Every intuition about "shortest paths" is backwards here, and only for timelike curves. For spacelike curves $\eta$ is indefinite on the variations and a straight line is neither maximum nor minimum. In curved spacetime the maximum is only local, up to unit 11's conjugate points.
The flat-space facts of this section, side by side with the Euclidean ones they reverse:
| Euclidean length | proper time | |
|---|---|---|
| straight line | shortest | longest |
| other extreme | no longest | no shortest |
| polygon form | $|x + y| \le |x| + |y|$ | $\lVert X + Y\rVert \ge \lVert X\rVert + \lVert Y\rVert$ |
26 · proper time
| method | structure it uses | Earth | traveller | where the asymmetry shows |
|---|---|---|---|---|
| proper time | length of a curve under $\eta$ | $10$ | $6$ | the traveller's worldline is bent; bent is shorter |
| radio counts | light cones and the Doppler factor $e^{\varphi} = 3$ | $10$ | $6$ | the flip: traveller's year $3$ of $6$, Earth's year $9$ of $10$ |
| simultaneity | hyperplanes $\eta$-orthogonal to the worldline | $10$ | $6$ | a $6.4$-year jump at the turn |
A group fixed by structure up to one speed, the quadratic form it preserves, and every effect — dilation, contraction, Doppler, causal order, the twins — is a property of that form.
Checks, all passed. $\gamma = 5/3$; rapidity $\ln 3$; Doppler factor $e^{\ln 3} = 3$; $1 + 9 = 10$, $3 + 3 = 6$; $1.8 + 6.4 + 1.8 = 10$; $\lVert(10,0)\rVert = 10 \ge 3 + 3$. As $c \to \infty$ every column reads $10$.
26 · checkpoint
On paper and without notes, you can:
A derivation that assumes $a = \gamma$ without reciprocity, or never shows $K$ is constant; a proper time with the wrong sign under the root or missing its $1/c$; a triangle inequality with no proof that $\eta(X, Y) < 0$.
27 relativistic dynamics, which needs 16 as well · 28 the field tensor, after 27 and 25 · 30 the equivalence principle, where the traveller's turn gets its own coordinates.