Embark on an immersive exploration from the exosphere to Earth's inner core, discovering the wonders of each unique layer.
600-10,000 km above Earth's surface
The exosphere is the outermost layer of Earth's atmosphere, where it gradually fades into the emptiness of space. In this rarified region, gas molecules are so far apart they rarely collide with each other.
The exosphere contains mainly hydrogen and helium, with some oxygen, nitrogen and carbon dioxide. Here, molecules with enough energy can actually escape Earth's gravity entirely and drift into space.
Exosphere Composition
2000°C
-120°C
85-600 km above Earth's surface
The thermosphere is where Earth's atmosphere begins to merge with outer space. Despite being incredibly thin, this layer absorbs the sun's high-energy X-rays and UV radiation, causing temperatures to soar to an astounding 2000°C.
Within this layer, gas molecules are so far apart that they can travel hundreds of kilometers without colliding with one another. This is also where you'll find charged particles forming the ionosphere, enabling radio wave transmission around the planet.
The stunning aurora borealis (northern lights) and aurora australis (southern lights) occur in the thermosphere when solar particles collide with oxygen and nitrogen atoms.
50-85 km above Earth's surface
The mesosphere is the third layer of Earth's atmosphere, positioned directly above the stratosphere and below the thermosphere. In this layer, temperatures decrease with altitude, reaching the coldest temperatures in Earth's atmosphere.
The mesosphere is where most meteors burn up upon entry into Earth's atmosphere, creating the brilliant streaks of light we call "shooting stars." The friction between the meteor and air molecules generates intense heat, vaporizing most meteors before they can reach the lower atmosphere.
Despite its critical protective function, the mesosphere is one of the least understood layers of our atmosphere as it's too high for aircraft and too low for satellites to explore directly.
These beautiful "night-shining" clouds occur in the upper mesosphere and are made of ice crystals. They can only be seen during astronomical twilight when the sun is below the horizon.
0°C
-90°C
-3°C
-50°C
10-50 km above Earth's surface
The stratosphere is a vital protective layer of Earth's atmosphere that contains the ozone layer. Unlike the troposphere below, temperatures in the stratosphere increase with altitude due to the absorption of ultraviolet radiation from the Sun.
The ozone layer within the stratosphere absorbs 97-99% of the Sun's high-frequency ultraviolet radiation, acting as a shield that protects life on Earth from harmful radiation. Without it, life as we know it could not exist on our planet's surface.
This stable layer is where commercial aircraft often fly to avoid turbulence, and where weather balloons can reach their maximum altitude before bursting from the reduced external pressure and gas expansion.
The ozone layer absorbs 97-99% of the Sun's medium-frequency ultraviolet light, which otherwise would potentially damage exposed life forms on Earth.
0-12 km above Earth's surface
The troposphere is the lowest layer of Earth's atmosphere and the one we call home. It contains approximately 75-80% of the atmosphere's mass and almost all of Earth's weather occurs within this dynamic layer.
Unlike the stratosphere above it, temperatures in the troposphere decrease with altitude, dropping about 6.5°C for every kilometer of altitude. This temperature gradient creates vertical currents and atmospheric mixing that powers our weather systems.
From towering cumulonimbus clouds to gentle rainfall, from turbulent thunderstorms to tranquil sunsets, the troposphere is where Earth's weather patterns develop, mature, and dissipate in an endless cycle.
The troposphere hosts all of Earth's weather. See various weather patterns in action:
-55°C
15°C
The Interface Between Atmosphere and Earth
Sea level marks the critical boundary between Earth's atmosphere and its solid/liquid surface. Covering approximately 71% of our planet's surface, oceans play a vital role in regulating temperature, generating oxygen, and supporting an incredible diversity of life.
The ocean is divided into different depth zones, each with its own unique ecosystem. The sunlit epipelagic zone (0-200m) receives enough sunlight for photosynthesis, while deeper zones transition into complete darkness where specialized creatures have evolved remarkable adaptations.
Oceans also serve as a massive carbon sink, absorbing nearly 30% of human-produced carbon dioxide and helping mitigate climate change. However, this absorption is causing ocean acidification, threatening marine ecosystems worldwide.
The sunlit surface zone where photosynthesis occurs. Home to phytoplankton, coral reefs, and many fish species.
The twilight zone with limited light. Features bioluminescent organisms and vertical daily migrations.
The midnight zone with no light. Home to bizarre creatures like anglerfish and giant squid.
The abyssal zone of extreme pressure. Features highly specialized deep-sea creatures.
71%
of Earth's surface
97%
of Earth's water
50%+
of world's oxygen
11km
deepest point
5-70 km thick outer layer
The Earth's crust is the thin, solid outermost layer of our planet, making up just 1% of Earth's total mass. This relatively brittle shell is where we live, build, and explore. It's divided into oceanic crust (thinner and denser) and continental crust (thicker and less dense).
The crust is not a single, continuous piece but is broken into tectonic plates that float on the semi-solid mantle below. The movement of these plates causes earthquakes, volcanic eruptions, and the formation of mountains when they collide.
Rich in minerals and elements, the crust provides the resources that sustain human civilization, from the metals we use to build our cities to the fossil fuels that power our industries.
The movement of tectonic plates creates different geological features at their boundaries:
Plates collide, forming mountains and volcanoes
Plates move apart, creating rifts and new crust
Plates slide past each other, causing earthquakes
20°C
500°C
46%
28%
8%
5%
4%
9%
2,900 km thick middle layer
The mantle is the thickest layer of Earth, making up approximately 84% of Earth's volume. This vast region between the crust and the core consists of hot, semi-solid rock called magma that slowly flows like an extremely viscous liquid.
The mantle is divided into several regions: the upper mantle including the asthenosphere, the transition zone, and the lower mantle. Heat from the core and radioactive decay drives convection currents within the mantle, where hotter material rises while cooler material sinks.
These convection currents are the driving force behind plate tectonics, causing the movement of Earth's crustal plates, and are responsible for volcanic eruptions when magma finds its way to the surface through weak points in the crust.
Includes the rigid lithosphere and ductile asthenosphere. The asthenosphere allows tectonic plates to move and is the primary source of magma for volcanoes.
Contains minerals undergoing phase transitions. Acts as a barrier to mixing between upper and lower mantle, influencing convection patterns.
Higher pressure causes minerals to pack more tightly. Slower convection here affects heat transfer from the core to the upper mantle.
500°C
4000°C
44%
23%
21%
6%
Primary minerals: Olivine, Pyroxene, Garnet, and their high-pressure forms
2,200 km thick liquid metal layer
The outer core is a 2,200 km thick layer of molten iron and nickel that surrounds Earth's inner core. This dynamic region of liquid metal is in constant turbulent motion, flowing and swirling with powerful currents.
The movement of electrically conductive material in the outer core generates Earth's magnetic field through a process called the geodynamo. This magnetic field extends far into space, creating a protective shield called the magnetosphere that deflects harmful solar radiation.
With temperatures ranging from approximately 4,000°C to 6,000°C and extreme pressures, the outer core exists in a liquid state despite these intense conditions. Its continuous motion is essential for maintaining Earth's magnetic field, which has been crucial for the development and protection of life on our planet.
The outer core generates Earth's magnetic field through a self-sustaining process:
Heat from the inner core causes the liquid metal in the outer core to rise, cool, and sink in a continuous cycle.
Earth's rotation causes the flowing metal to twist into spiraling currents, creating a complex flow pattern.
The movement of electrically conductive fluid across existing magnetic field lines generates electric currents that reinforce the magnetic field.
4000°C
6000°C
80%
5%
15%
Density
9,900-12,200 kg/m³
Pressure
135-330 GPa
1,220 km radius solid metal sphere
At the very center of our planet lies the inner core, a solid sphere of iron and nickel approximately 1,220 kilometers in radius. Despite the crushing pressure and extreme temperatures exceeding 5,000°C (hotter than the surface of the Sun), the inner core remains solid due to the immense pressure.
Discovered in 1936 by seismologist Inge Lehmann, the inner core rotates slightly faster than the rest of the planet in what scientists call super-rotation. This differential rotation may contribute to the generation of Earth's magnetic field in conjunction with the liquid outer core.
Recent research suggests the inner core might have a complex structure, with different crystalline properties in distinct regions, and possibly even an innermost inner core with different properties. As Earth's deepest and most inaccessible layer, it continues to challenge our understanding of the planet.
The inner core has a complex crystalline structure of iron atoms arranged in a hexagonal close-packed pattern, giving it unique physical properties.
The inner core rotates slightly faster than the rest of Earth, completing an extra rotation every 900-1,000 years. This differential rotation is influenced by the magnetic and gravitational forces from the mantle.
Seismic waves travel faster through the inner core in a north-south direction than east-west, indicating alignment of iron crystals that suggests complex formation processes.
85%
10%
5%
Density
12,600-13,000 kg/m³
Age
~1-1.5 billion years
Did You Know?
If you could travel from Earth's surface to the inner core, you would need to journey 6,371 kilometers (3,958 miles) — about the same as traveling from New York to Los Angeles and back!
You've explored all layers of our planet, from the outermost reaches of the exosphere to the very center of the inner core.
Explore the scientific inspiration and educational purpose behind this interactive exploration of Earth's layers.
This interactive experience was designed to make Earth science accessible and engaging to learners of all ages. By visualizing complex geological and atmospheric concepts, we aim to inspire curiosity about our planet's structure.
All visualizations and information presented are based on current scientific understanding. We've collaborated with geologists, atmospheric scientists, and educators to ensure accuracy while making the content approachable and intuitive.
Inspired by the breathtaking animation style of Studio Ghibli, our visual approach combines scientific accuracy with artistic expression. This aesthetic choice creates an immersive experience that evokes wonder while maintaining educational integrity.
Lead Geophysicist
Provided expert guidance on Earth's internal structure and ensured scientific accuracy throughout the project.
Atmospheric Scientist
Specialized in atmospheric layer dynamics and weather patterns to accurately represent Earth's outer layers.
Lead Designer
Created the visually stunning animations and interface inspired by Ghibli's aesthetic sensibilities.
Educational Consultant
Ensured content is engaging and accessible for students across different age groups and educational settings.
Have questions about Earth's layers or interested in using our presentation? We'd love to hear from you.