Equations · equation

FLRW Metric

Cosmology · 1935

Equation
ds² = −c²dt² + a(t)²[dr²/(1 − kr²) + r²(dθ² + sin²θ dφ²)]
Field
Cosmology
Named After
Friedmann · Lemaître · Robertson · Walker
Year
1935

Symbols

ds the spacetime interval · t cosmic time · r, θ, φ comoving coordinates that expand with space · a(t) the scale factor · k spatial curvature (−1 open, 0 flat, +1 closed) · c speed of light

Significance

The shape of the universe, written down. Assume only that space is homogeneous and isotropic — the same everywhere, the same in every direction — and this is the *only* geometry allowed; that uniqueness is a theorem, not a modelling choice. Everything else in cosmology follows: feed this metric to Einstein's field equations and the Friedmann equations fall out, and the redshift-distance relation with them. All the physics hides in one function of time, a(t), and one number, k.

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From the Equations database in Notion, last edited 2026-08-26. This page is the row, rendered by the build; nothing on it is written by hand.