Always falling. Never landing.
Gravity pulls planets toward the Sun while their sideways motion carries them onward. All eight orbit counterclockwise when viewed from above the north side of the orbital plane.
Solar System INTERACTIVE 3D
One star. Eight worlds. A whole new perspective.
OUR COSMIC NEIGHBORHOOD
Illustrative scale & timing ↗Choose a world. Follow its story.
Compressed time · not live positions
Drag to orbit · Scroll / pinch to zoom · Right-drag / two fingers to pan
A day is a turn.
Rotation is a world spinning on its axis; revolution is its journey around the Sun. The facts panel lists sidereal rotation, measured against distant stars, rather than sunrise to sunrise.
Rocky inside. Giant outside.
Mercury, Venus, Earth and Mars have solid, rocky surfaces. Beyond them are the gas giants Jupiter and Saturn, then the ice giants Uranus and Neptune.
How the Solar System works
The Solar System is the Sun and the collection of worlds held around it by gravity. It includes eight planets, their moons, dwarf planets, asteroids, comets and smaller material. Our interactive explorer focuses on the Sun, all eight planets and Earth’s Moon, so you can connect the movements you see with the ideas explained below.
What keeps planets in orbit?
An orbit is the curved path one body follows around another under gravity. The Sun pulls each planet inward, while the planet’s sideways motion carries it onward. Together, these produce a continuing journey around the Sun. A planet does not need an engine to keep moving through space.
Planets nearer the Sun travel around it more quickly and follow shorter paths, so their years are shorter. Mercury completes an orbit in about 88 Earth days; Neptune needs nearly 165 Earth years. Our animation compresses those timings so both movements are visible.
The eight planets in order
From the Sun outward, the planets are Mercury, Venus, Earth, Mars, Jupiter, Saturn, Uranus and Neptune. The first four are rocky planets with solid surfaces. Jupiter and Saturn are gas giants, while Uranus and Neptune are ice giants.
“Ice giant” describes a difference in composition, not a frozen surface you could stand on. These outer planets are very different from the rocky ground of Earth or Mars. Use the planet facts below to compare their sizes and orbital periods.
Why a day and a year are different
Rotation means spinning on an axis. Revolution means completing an orbit. Earth spins roughly once in 24 hours but takes about 365 days to travel around the Sun. These are separate motions, so a planet can have a short day and a very long year.
The facts here use sidereal rotation: one turn measured against distant stars. That can differ from the time between sunrises because the planet is also moving around the Sun. Venus rotates in the opposite direction to most planets, and Uranus turns almost on its side.
Why planets have different environments
Distance from the Sun matters, but it does not explain a planet’s environment on its own. Atmosphere also affects how heat is absorbed, retained and redistributed. Venus is hotter at its surface than Mercury even though Venus is farther from the Sun, because its dense atmosphere traps heat.
Earth has oceans and an atmosphere that support the life we know. Mars has a thin atmosphere and a cold, dry surface. Comparing these nearby rocky worlds shows why size, distance and atmosphere must be considered together.
How moons and rings fit into the system
A moon is a natural satellite that orbits a planet or another body. Earth’s Moon travels around Earth while both travel around the Sun. The Moon spins once per orbit, which is why nearly the same side faces Earth.
Saturn’s rings are made of many separate pieces of ice and rock, each orbiting the planet. They are not a solid sheet. This model draws simplified bands to show their overall shape; other giant planets also have rings, but those fainter systems are omitted here.
How to read this 3D Solar System
Start with the whole system, then select a planet to follow it. Pause to compare worlds, turn orbital paths on to trace their journeys, and change the speed to watch motion at a comfortable pace. Reset the camera to return to the overview.
The model preserves planet order and the common orbital direction, viewed from the north side of the orbital plane. Sizes, spacing, starting positions and timing are illustrative. It is a learning model rather than a display of where the planets are today.
Model simplifications & image credit
A map for understanding, not navigation.
Planet sizes and orbital distances use separate illustrative scales. The Sun is greatly reduced relative to the planets, small worlds are enlarged, and outer orbits are compressed. Earth’s Moon is enlarged and placed closer than a common scale would allow.
Orbits are circular and coplanar rather than elliptical and inclined. All advance counterclockwise viewed from ecliptic north. Starting angles are arbitrary: these are not accurate real-time planetary positions.
At 1×, Mercury orbits in 28 seconds and Neptune in about 198 seconds. Periods follow 28 × (real orbital days / 88)0.3, preserving which planets orbit faster but not their true period ratios. Spins are independently compressed: most turn in about 17 seconds, Mercury and Venus in about 52. Axial tilt magnitudes are approximate; their compass directions are illustrative. Tilt represents retrograde rotation for Venus and Uranus.
The Moon completes one orbit and spin in 10 seconds, keeping the same side toward Earth. Its orbital inclination is omitted. Saturn’s rings have simplified gaps and opacity; other rings, moons, dwarf planets, asteroids, eclipses and mutual gravitational effects are omitted. Ambient lighting makes night sides easier to see. Stars are decorative, not a sky chart. The Sun’s glow and colors are illustrative.
Image credit & fact checking
Explanations are written for HowItWorks3D. Rounded figures were checked against NASA Science resources on October 4, 2026; detailed source records are retained in the project documentation. This independent educational model is not endorsed by NASA.
Earth map: NASA Earth Observatory, Blue Marble: Next Generation, December 2004, with shaded topography and bathymetry. Resized for this model; an historical composite, not live imagery. Original source ↗ . NASA source imagery is excluded from the site ownership claim. All other surface textures are original procedural illustrations, not photographic maps.
Sun and planet facts: a world-by-world reference
Meet the worlds in order from the Sun. These real-world facts describe each body; the 3D view uses enlarged planets and compressed distances to make them easier to explore.
Sun
A star powered by nuclear fusion. Its gravity holds this planetary system together.
- Mean diameter
- 1.4 million km
- Orbital period
- —
- Sidereal rotation
- ~25 days at equator
- Mean solar distance
- System center
In its core, hydrogen fuses into helium and releases energy. The Sun is plasma, so its equator and poles rotate at different rates; this model uses one uniform spin.
Mercury
The smallest planet and the closest to the Sun. Its cratered surface records billions of years of impacts.
- Mean diameter
- 4,880 km
- Orbital period
- 88 Earth days
- Sidereal rotation
- 58.6 Earth days
- Mean solar distance
- 0.39 AU
Mercury has only a very thin exosphere. With little atmosphere to redistribute heat, its days are extremely hot and its nights extremely cold.
Venus
A rocky world wrapped in thick clouds, with the hottest surface of any planet.
- Mean diameter
- 12,104 km
- Orbital period
- 224.7 Earth days
- Sidereal rotation
- 243 Earth days
- Mean solar distance
- 0.72 AU
Its carbon-dioxide atmosphere traps heat through a powerful greenhouse effect. Venus spins retrograde: opposite to most planets. The texture shows illustrative clouds, not its hidden ground.
Earth
Our ocean-covered home is the only world currently known to support life.
- Mean diameter
- 12,742 km
- Orbital period
- 365.25 Earth days
- Sidereal rotation
- 23.9 hours
- Mean solar distance
- 1 AU
Earth’s tilted axis causes the seasons as it orbits the Sun. Its Moon rotates once per orbit, keeping nearly the same face toward Earth. Select Earth to follow both worlds.
Mars
A cold desert world with rusty soil, polar ice, and evidence of ancient rivers and lakes.
- Mean diameter
- 6,779 km
- Orbital period
- 687 Earth days
- Sidereal rotation
- 24.6 hours
- Mean solar distance
- 1.52 AU
Iron minerals oxidize in the soil, giving Mars its reddish appearance. Its thin atmosphere cannot sustain widespread liquid water on the surface today.
Jupiter
The largest planet. Bands of clouds and powerful storms sweep around a deep hydrogen-and-helium atmosphere.
- Mean diameter
- 139,820 km
- Orbital period
- 11.9 Earth years
- Sidereal rotation
- 9.9 hours
- Mean solar distance
- 5.20 AU
Jupiter has no solid surface like Earth’s. Its Great Red Spot is a long-lived storm. The painted bands and storm here are illustrative, not current weather.
Saturn
A gas giant surrounded by an enormous system of icy rings.
- Mean diameter
- 116,460 km
- Orbital period
- 29.4 Earth years
- Sidereal rotation
- ~10.7 hours
- Mean solar distance
- 9.58 AU
The rings are countless separate pieces of ice and rock, not a solid disk. Their widths and gaps are simplified here. Other giant planets also have faint rings, omitted in this view.
Uranus
An ice giant that rotates nearly on its side, with an axis tilted about 98 degrees.
- Mean diameter
- 50,724 km
- Orbital period
- 84 Earth years
- Sidereal rotation
- 17.2 hours
- Mean solar distance
- 19.2 AU
Methane absorbs red light in its atmosphere, helping give Uranus its blue-green color. Its extreme tilt produces unusual seasons. The axis direction here is illustrative.
Neptune
The outermost planet, a cold ice giant with a dynamic atmosphere and powerful winds.
- Mean diameter
- 49,244 km
- Orbital period
- 164.8 Earth years
- Sidereal rotation
- 16.1 hours
- Mean solar distance
- 30.1 AU
Neptune takes nearly 165 Earth years to circle the Sun. Its color is stylized here for recognition; actual appearance depends on image processing and viewing conditions.