ORBIT Solar System Explorer

Natural satellite Ariel

Ariel

Canyons trace a reshaped icy surface

Crossing canyons and grooves cover its surface. Relatively few huge craters suggest parts of the terrain were resurfaced.

Rendered view of Ariel
Illustrative lighting and viewpoint · Image credits
Mean radius
578.9 km
Mean diameter
1,157.8 km
Orbital semimajor axis
190,929 km

01 / Overview

Meet Ariel

Ariel is one of Uranus's brighter major moons, with extensive canyons and regions relatively poor in large craters. Its history includes crustal deformation or renewal as well as impacts. Comparing canyons with surrounding older terrain helps establish the relative sequence of those changes.

02 / Key data

Core parameters

Mean radius
578.9 km
Mean diameter
1,157.8 km
Orbital semimajor axis
190,929 km
Orbital period
2.52 d
Parent planet
Uranus
Data and calculation notes

Radii are mean values; orbital data describe each world’s scale and motion.

03 / Further reading

A closer look

What makes this world distinctive5
  • William Lassell discovered Ariel in 1851.

  • Ariel has extensive canyon systems.

  • Ariel is one of the brighter major Uranian moons.

  • Some areas on Ariel have fewer craters, suggesting past geological resurfacing.

  • Voyager 2 observed Ariel during its 1986 flyby.

Gravity and the interior14
  • A natural satellite forms naturally and orbits a larger body; an artificial satellite is built by people.

  • Tidal locking matches rotation to orbital motion; it does not mean no rotation.

  • A moon's orbit need not lie in the same plane as its planet's orbit around the Sun.

  • Differences in gravity across a moon can deform it through tides.

  • Repeated tidal deformation can turn orbital energy into internal heat.

  • Orbital resonance means periods near simple integer ratios, allowing repeated pulls between moons to build up.

  • Some moons formed in discs around planets; others may have been captured later.

  • Small moons are often irregular because their gravity cannot overcome the strength of their materials.

  • Large moons tend to be rounder because gravity shapes them.

  • Icy moons may have liquid oceans under their shells; a frozen surface does not mean a fully frozen interior.

  • Finding water or organic molecules is not the same as finding life.

  • A planet and moon both orbit their common center of mass; the heavier body's wobble is usually smaller.

  • Other bodies perturb a moon's orbit; a fixed ellipse is only an approximation.

  • Moons can be larger than some planets; classification is not based on diameter alone.

Surface and observation11
  • Crossing canyons and grooves cover its surface. Relatively few huge craters suggest parts of the terrain were resurfaced.

  • A moon's visible brightness usually comes from reflected sunlight.

  • Moons have sunlit and dark sides too; the side facing away from the planet is not permanently dark.

  • Crater counts help estimate surface ages, but resurfacing and the impact environment also matter.

  • A moon hiding a background star causes an occultation, useful for measuring size or probing an atmosphere.

  • A moon entering its planet's shadow experiences an eclipse, depending on the orbits' spatial alignment.

  • Tiny changes in a spacecraft's speed can reveal a moon's mass and gravity field.

  • Composition, grain size, and lighting all affect surface color; enhanced-color images differ from naked-eye views.

  • The day–night boundary is the terminator; long shadows nearby bring out terrain.

  • Surfaces with little or no atmosphere lack strong weather erosion and preserve old impact scars more easily.

  • A moon's observed phases come from changing angles between the Sun, moon, and observer.

04 / Sources

Trusted sources

NASA Science — ArielJPL — Orbital data

Image credits

Images reproject and light existing textures; they are not live observations.

Surface texture:ItzImcool; Paul Schenk; NASA/JPL/Ted Stryk · License · Rendered by ORBIT

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