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Sandbox Physics

Gravitational waves · laser interferometry

LIGO · Listening to Spacetime

Fly through a virtual LIGO detector: watch freely falling masses breathe with a gravitational wave, enter the perpendicular four-kilometre arms, follow split laser beams as they return and cancel, then see two observatories confirm a black-hole merger together.

Interactive modelLIGO · Listening to Spacetime
Current scene1 · Spacetime strain
What changesProper distance
Signalh(t)

CONTINUE EXPLORING

Understand, then measure

How does a tiny arm-length change become a signal at the output?

Scientific explanation

Read the picture as a physical process

What is happening

Why does the ring of masses become an ellipse?

Treat the dots as disconnected test masses in free fall. A gravitational wave arriving perpendicular to the ring does not blow them outward; it changes their proper separations. Plus polarization stretches one transverse axis while squeezing the other. Cross polarization is the same pattern rotated by 45 degrees.

Causal chain

  1. 1
    The wave passesThe transverse spacetime metric oscillates
  2. 2
    Distances changex grows while y shrinks
  3. 3
    The ring deformsThe long and short axes swap half a cycle later

Mathematical model

Lx(t)≈L[1+12h+(t)]Ly(t)≈L[1−12h+(t)]\begin{aligned} L_x(t) &\approx L\left[1 + \frac{1}{2}h_{+}(t)\right] \\ L_y(t) &\approx L\left[1 - \frac{1}{2}h_{+}(t)\right] \end{aligned}

Symbols

LL
Reference separation with no wave
h+(t)h_{+}(t)
Dimensionless plus-polarized strain
Lx, LyL_x,\,L_y
Proper separations along two transverse axes

Model boundaryThis is the standard long-wavelength, TT-gauge teaching picture. The animation exaggerates strain by roughly 10²⁰. Coordinate positions may remain fixed while proper distances change.

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