Physical · the experiment

Farthest in July

Earth is closest to the Sun in January and farthest in July — the exact opposite of what "distance makes the seasons" would predict. This page went up on 6 July 2026, the very day Earth reached aphelion, its greatest distance from the Sun all year, in the middle of northern summer.

Nearly everyone, asked why summer is hot, reaches for the intuitive answer: the Earth must be closer to the Sun. It isn't. When it's summer in New York, London, and Tokyo, the Earth is at its farthest point of the entire orbit. The real cause is the 23.4° tilt of Earth's axis — and you can prove it below by switching each effect off and watching which one the seasons actually depend on.

The orbit, from above — the axis keeps a fixed direction in space

The Sun's daily energy, recomputed live

Distance to Sun
152.1M km
aphelion — farthest
Sunlight intensity
96.7%
of the year's average (∝ 1/distance²)
Noon Sun height
73.4°
above the horizon
Daylight length
15.0 h
sun up
Daily sunlight energy at this latitude (top of atmosphere)
483 W/m²
24-hour average · this is the forcing that drives the season

A whole year of daily sunlight at your latitude

what you get now distance effect alone
Tilt on, orbit elliptical: summer delivers 3.1× the winter sunlight. Turn the tilt off and the swing collapses to the thin dashed line — the pure distance effect, which for the north peaks in January. The seasons are the tilt.

Here is the whole argument in one move. Uncheck Axial tilt: the tall seasonal curve collapses onto the thin dashed line. That dashed line is everything the changing distance does by itself — a faint ripple of a few percent that, for the Northern Hemisphere, is strongest in January, the depth of winter. Now re-check the tilt and uncheck Elliptical orbit instead, pretending Earth circles the Sun at a fixed distance: the seasonal curve barely flinches. One switch controls the seasons. The other barely matters — and points the wrong way.

Why the tilt does so much

The tilt changes sunlight two ways at once, and they compound. In your summer, your hemisphere leans toward the Sun, so the noon Sun climbs higher — its rays strike the ground closer to straight-on instead of smearing across a slanted surface — and the day is longer, so that stronger sunlight falls for more hours. High sun × long day is summer. Low sun × short day is winter. At 40° N the top-of-atmosphere sunlight runs about 483 W/m² in June and 156 W/m² in December — a factor of three, all from the tilt.

The distance, meanwhile, varies the total sunlight by only about 6.9% across the year (the orbit is very nearly a circle — its off-roundness is about 1 part in 60). And because Earth happens to be closest in January, that small effect actually makes northern winters a touch milder and southern summers a touch fiercer — a real, measurable, second-order nudge riding on top of the tilt, never competing with it.

The check — every number here is recomputed, not asserted

The daily sunlight is the standard top-of-atmosphere daily-mean insolation Q = (S₀/π)·(a/r)²·[H₀·sinφ·sinδ + cosφ·cosδ·sinH₀] (Hartmann, Global Physical Climatology, eq. 2.20), computed in your browser from the same code as the repository's verifier. The verifier reproduces the textbook anchor values, which is how we know the formula is right:

Full computation, sources, and the honest limits: research/seasons/verify.mjs and research/seasons/facts.md. Constants: S₀ = 1361 W/m² (Kopp & Lean 2011), tilt 23.44°, aphelion 152.09M km on 6 Jul 2026 (EarthSky / In-The-Sky.org), perihelion 147.10M km (NASA).