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Spacetime Diagrams

Spacetime diagrams (Minkowski diagrams) are the geometric language of special relativity. Each point is an event; each particle traces a worldline; light travels at 45°. The causal structure — what can influence what — is encoded in the light cone.

Key Concepts

Worldline
The path of an object through spacetime: a curve (t,x(t))(t,x(t)) in the tt-xx plane. A particle at rest is a vertical line; one moving at constant velocity is a straight line; light travels at 45° (slope cc).
Light Cone
The set of events connected to a given event by light signals. The future light cone contains all events that can be influenced; the past light cone all events that could have influenced. Events outside the light cone are causally disconnected.
Hyperbolic Geometry
Lorentz boosts are hyperbolic rotations in Minkowski space. Lines of constant proper time are hyperbolas; the Lorentz-boosted axes tilt toward the light cone (they always straddle it symmetrically).
Proper Time from Diagram
The proper time along a worldline segment is Δτ=Δt2Δx2/c2\Delta\tau=\sqrt{\Delta t^2-\Delta x^2/c^2} — the "length" of the worldline in Minkowski metric (using the ++--- convention).

Key Equations

Worldline slope
slope=c/v=c/βc=1/β\text{slope} = c/v = c/\beta c = 1/\beta
In a ct vs x diagram, the slope is c/v; light has slope 1 (at 45°).
Proper time (segment)
Δτ=Δt2Δx2/c2=Δt/γ\Delta\tau = \sqrt{\Delta t^2 - \Delta x^2/c^2} = \Delta t/\gamma
The "length" of a worldline segment; shorter than coordinate time Δt.
Light cone
ct=±xct = \pm x
Light cone boundary; timelike events have |ct| > |x|; spacelike have |ct| < |x|.
Worked Example

Reading Proper Time from a Spacetime Diagram

Problem

A worldline passes through events A=(t=0,x=0)A=(t=0,x=0) and B=(t=5 ns,x=1.2 m)B=(t=5\text{ ns}, x=1.2\text{ m}) (c=3×108c=3\times10^8 m/s). Find the proper time Δτ\Delta\tau between them.

Solution

Convert: cΔt=3×108×5×109=1.5c\Delta t=3\times10^8\times5\times10^{-9}=1.5 m.

Δτ=Δt2Δx2/c2=1c(cΔt)2Δx2\Delta\tau = \sqrt{\Delta t^2 - \Delta x^2/c^2} = \frac{1}{c}\sqrt{(c\Delta t)^2 - \Delta x^2}
Δτ=1c1.521.22=1c2.251.44=0.81c=0.9 m3×108 m/s=3 ns\Delta\tau = \frac{1}{c}\sqrt{1.5^2 - 1.2^2} = \frac{1}{c}\sqrt{2.25-1.44} = \frac{\sqrt{0.81}}{c} = \frac{0.9\text{ m}}{3\times10^8\text{ m/s}} = 3\text{ ns}
Answer Δτ=3.0\Delta\tau=3.0 ns.
Practice

Exercises

7 problems
1 of 7

A particle moves at v=0.60cv=0.60c. What is the slope of its worldline (in a ctct vs xx diagram)?

(dimensionless)
2 of 7

Events A=(ct=0,x=0)A=(ct=0,x=0) and B=(ct=5 m,x=3 m)B=(ct=5\text{ m},x=3\text{ m}). Find the proper time Δτ\Delta\tau (in m/c, or equivalently in units where c=1). Δτ2=(5)2(3)2\Delta\tau^2=(5)^2-(3)^2.

m/c
3 of 7

Is the interval between events A=(ct=3 m,x=5 m)A=(ct=3\text{ m},x=5\text{ m}) and B=(ct=0,x=0)B=(ct=0,x=0) timelike, lightlike, or spacelike? Find s2=(cΔt)2Δx2s^2=(c\Delta t)^2-\Delta x^2.

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4 of 7

A rocket leaves Earth at t=0t=0 at v=0.80cv=0.80c. How far (in ly) from Earth is it when the Earth clock reads t=5.0t=5.0 yr?

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5 of 7

Two flashes occur at (ct=0,x=0)(ct=0,x=0) and (ct=4,x=2)(ct=4,x=2) m. A third observer sees them at the same time (Δt=0\Delta t'=0). At what speed vv (as fraction of cc) must this observer move? v/c=cΔt/Δxv/c=c\Delta t/\Delta x.

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6 of 7

Light from a star 10 ly away was emitted when? Looking at the past light cone, light emitted 10 yr ago arrives now. If the star is now 10 ly away, how many years ago was the light emitted?

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7 of 7

A spaceship accelerates with proper acceleration a=10a=10 m/s² (1g). The Rindler horizon is at distance c2/ac^2/a behind the ship. Find this distance (in light-years). (c2/a=9×1016/10=9×1015c^2/a=9\times10^{16}/10=9\times10^{15} m; 1 ly =9.46×1015=9.46\times10^{15} m.)

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Key Takeaways

  • Spacetime diagrams visualize events, worldlines, and causality. Light travels at 45°; massive particles always have |slope| > 1.
  • The light cone divides spacetime into timelike future/past (can be influenced/can influence) and spacelike elsewhere (causally disconnected).
  • Proper time is the "length" of a worldline: Δτ=Δt2Δx2/c2\Delta\tau=\sqrt{\Delta t^2-\Delta x^2/c^2}.
  • A Lorentz boost tilts the ctct' and xx' axes symmetrically toward the light cone — lengths and times change, but the light cone is invariant.