# Perihelion and aphelion

The perihelion (/ˌpɛrɪˈhiːliən/) of any orbit of a celestial body about the Sun is the point where the body comes closest to the Sun. It is the opposite of aphelion (/æpˈhiːliən/), which is the point in the orbit where the celestial body is farthest from the Sun.[1]

The perihelion and aphelion are the nearest and farthest points respectively (apsides) of a body's direct orbit around the Sun.

## Etymology

The words perihelion and aphelion were coined by Johannes Kepler[2] to describe the orbital motion of the planets. The words are formed from the prefixes peri- (Greek: περί, near) and apo- (Greek: ἀπό, away from) affixed to the Greek word for the sun, ἥλιος.[3]

Perihelion and aphelion are sometimes incorrectly used for the orbits of objects about bodies other than the Sun. The correct terms are:

• For orbits around the Earth: perigee and apogee.
• For orbits around a star: periastron and apastron.
• For orbits around any center of mass: periapsis (or pericenter) and apoapsis (or apocenter).

## Astronomical meaning

According to Kepler's first law of planetary motion, all planets, comets, and asteroids in the Solar System have approximately elliptical orbits around the Sun.[4] Newton's and Einstein's laws of gravity imply that the orbits are only approximately elliptical because of perturbations due to the gravitational attraction of other bodies. Every ellipse has two focus points, and the Sun is at one of these focus points for the elliptical orbits of its satellites. Hence, an orbiting body has a closest and a farthest point from its parent object, that is, a perihelion and an aphelion. Each extreme is known as an apsis.

Orbital eccentricity measures the flatness (departure from a perfect circle) of the orbit.

## Application to Earth

Earth is about 147.1 million kilometers (91.4 million miles) from the Sun at perihelion around January 3, in contrast to about 152.1 million kilometers (94.5 million miles) at aphelion around July 4 — a difference of about 5.0 million kilometers (3.1 million miles). (These dates change over time due to precession and other orbital factors, which follow cyclical patterns known as Milankovitch cycles. For a table of these dates for various years, see Apsis.)

Because of the increased distance at aphelion, only 93.55% of the solar radiation from the Sun falls on a given area of land as does at perihelion. However, this fluctuation does not account for the seasons,[5] as it is summer in the northern hemisphere when it is winter in the southern hemisphere and vice versa. Instead, seasons result from the tilt of Earth's axis, which is 23.4 degrees away from perpendicular to the plane of Earth's orbit around the sun. Winter falls on the hemisphere where sunlight strikes least directly, and summer falls where sunlight strikes most directly, regardless of the Earth's distance from the Sun.

In the northern hemisphere, summer occurs at the same time as aphelion. Despite this, there are larger land masses in the northern hemisphere, which are easier to heat than the seas. Consequently, summers are 2.3 °C (4 °F) warmer in the northern hemisphere than in the southern hemisphere under similar conditions.[6]