Earth Axial Tilt (Obliquity of the Ecliptic)

ε=0.4090928 rad\varepsilon = 0.4090928\ \text{rad}
Value0.4090928 rad
StatusConventional / typical value
SourceIAU 2006 precession model, epoch J2000 (slowly variable)
CategoriesAstronomical
Earth Axial Tilt (Obliquity of the Ecliptic) in every angle unit
microarcsecond84,381,447,000 μas
milliarcsecond84,381,447 mas
microradian409,092.8 μrad
arcsecond84,381.447 ″
arcminute1,406.3575 ′
mil (NATO)416.6985 mil
milliradian409.0928 mrad
gradian26.043657 gon
degree23.439291 °
compass point2.0834925 point
hour angle1.5626194 h
radian0.4090928 rad
quadrant0.26043657 quad
revolution0.065109141 rev

Learning zone

Seasons come from this angle, not from the varying distance to the Sun: the tilt points the northern hemisphere sunward in June and away in December, changing both the height of the Sun and the length of the day. The tilt fixes the tropics at 23.44° latitude, where the Sun can stand overhead, and the polar circles at 66.56°, where it can stay up all day. Eratosthenes measured the obliquity around 230 BC to within a fraction of a degree by comparing midsummer and midwinter shadows.

It is slowly changing. Planetary perturbations rock the obliquity between about 22.1° and 24.5° over a 41 000-year cycle — currently decreasing by roughly 47 arcseconds per century — and that cycle is one of the Milanković pacemakers of glaciation. The Moon's stabilising torque keeps the swing small; without it, models suggest Earth's tilt would wander chaotically like Mars's has.