Equations · equation

Kepler's First Law

Celestial Mechanics · 1609

Equation
r = p / (1 + e·cos θ)
Field
Celestial Mechanics
Named After
Johannes Kepler
Symbols
r distance from the Sun · p semi-latus rectum (size of the orbit) · e eccentricity (0 circle, <1 ellipse) · θ angle from closest approach
Year
1609

Significance

Planets travel ellipses with the Sun at one focus — not the perfect circles two millennia of astronomy had insisted on. Kepler got there through Tycho's data and eight arcminutes of Martian residual he refused to round away. The ellipse is not a fact about the solar system: an inverse-square attraction is one of only two force laws whose bound orbits close on themselves at all, so the shape falls out of Newton's law rather than having to be assumed. Written here as the polar equation of the orbit.

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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.