Earth’s Interior, Geology, and Atmosphere: Key Facts

Apr 14, 2026

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The planet’s interior consists of a solid inner core, a liquid outer core, a thick mantle, and a thin crust. The inner core is a solid sphere about 1,200 km in radius composed mainly of iron and nickel, while the outer core surrounds it as a 2,200 km‑thick liquid layer of the same metals. Above the core lies the mantle, a 2,900 km‑thick zone that behaves like very thick hot plastic, flowing slowly over geologic time. The crust forms the outermost solid shell, broken into plates; oceanic crust averages five kilometres thick, whereas continental crust ranges from 30 to 50 km.

Geologic and Magnetic Mechanisms

Heat left over from Earth’s formation, gravitational contraction, radioactive decay, and friction from sinking dense material fuels mantle convection. Warm mantle material rises, cools, and sinks, driving the motion of tectonic plates at a pace comparable to fingernail growth—only a few centimetres per year. Plate movement creates volcanism at boundaries and hot spots such as Hawaii, releasing gases that replenish the atmosphere.

The liquid outer core conducts electricity and convects, generating Earth’s magnetic field. Rotation organizes the convective flow into cylindrical rolls aligned with the spin axis, producing a bar‑magnet‑like field that deflects solar‑wind particles. This magnetic shield prevents atmospheric erosion, a process that stripped Mars of its air, and also channels some solar particles into the upper atmosphere, creating aurorae around 150 km altitude.

Atmospheric Composition and Dynamics

The atmosphere is dominated by 78 % nitrogen, 21 % oxygen, 1 % argon, and trace gases, including carbon dioxide at 0.04 %. The Kármán line at 100 km marks the conventional boundary of space. An ozone layer near 25 km absorbs harmful ultraviolet radiation. The greenhouse effect, primarily driven by CO₂, traps infrared radiation and keeps Earth from becoming an “iceball.”

Surface Conditions

Water covers roughly 70 % of the planet’s surface, likely delivered during formation and by comet or asteroid impacts. Human activity since the Industrial Revolution has raised atmospheric CO₂, melting glaciers, raising sea levels, and acidifying oceans. The combined influence of internal heat, plate tectonics, magnetic shielding, and atmospheric composition sustains the climate conditions that support life.

Takeaways

Earth’s interior comprises a solid inner core, a liquid outer core, a plastic‑like mantle, and a thin crust that forms tectonic plates.
Mantle convection, powered by residual heat and radioactive decay, drives plate movement at a rate similar to fingernail growth.
The liquid outer core’s convective motion creates a magnetic field that shields the atmosphere from solar‑wind erosion and produces aurorae.
The atmosphere’s nitrogen‑oxygen mix and a thin CO₂ layer generate a greenhouse effect that prevents the planet from freezing over.
Rising CO₂ from industrial activity is melting glaciers, raising sea levels, and acidifying oceans, altering Earth’s climate balance.

Frequently Asked Questions

How does mantle convection drive plate tectonics?

Mantle convection transports heat from the core upward, causing hot material to rise and cooler material to sink. This circulation creates shear forces that push against the overlying crust, sliding tectonic plates at a few centimetres per year and triggering earthquakes and volcanism.

Why is Earth’s magnetic field essential for atmospheric protection?

The magnetic field deflects charged particles in the solar wind, preventing them from stripping away atmospheric gases. Without this shield, the atmosphere would erode over time, as observed on Mars, and the planet would lose the conditions needed for life.

Does this page include the full transcript of the video?

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Helpful resources related to this video

If you want to practice or explore the concepts discussed in the video, these commonly used tools may help.

Geology Of Earth Educational Globe Model Recommended

A physical globe showing internal layers helps visualize the core, mantle, and crust structure described in the lecture.

Amazon →

Plate Tectonics Educational Science Kit

Hands-on models demonstrate how mantle convection and plate movement function, reinforcing the lecture's explanation of geologic dynamics.

Amazon →

Earth Science Reference Book For Students

Provides comprehensive diagrams and data on atmospheric layers, the greenhouse effect, and planetary structure for deeper study.

Amazon →

Magnetic Field Science Experiment Kit

Allows for the observation of magnetic fields and charged particle interactions, illustrating how Earth's core protects the atmosphere.

Amazon →

Links may be affiliate links. We only include resources that are genuinely relevant to the topic.

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Full Transcript YouTube

The Earth is a planet.
That’s a profound statement, and one that’s
not really all that obvious. For thousands
of years, planets were just bright lights
in the sky, one-dimensional points that wandered
among the fixed stars. How could the Earth
be one of them?
With the invention of the telescope those dots
became worlds, and with spacecraft they became
places. The Earth went from being our unique home
in the Universe to one of many such…well, planets.
The Earth is the largest of the terrestrial
planets, the four smaller, denser, rocky worlds
orbiting close in to the Sun. It’s about
13,000 kilometers across, and has a single,
large Moon which we’ll learn a lot more
about next week.
Unlike the other three terrestrial planets,
Earth has something very important: Water.
Or, more specifically, liquid water on its
surface, where it can flow around, evaporate,
become clouds, rain down, and then mix up
chemicals so they can do interesting, complex
things—like support life.
Earth’s ability to sustain life depends
on that water. It also depends on Earth’s
atmosphere, of course—breathing has its
advantages—and both, weirdly enough, depend
on Earth’s magnetic field to exist. And
that, in turn, depends on what’s going on
deep inside our planet. So, let’s take a
look.
Like the Sun, the Earth is a many-layered
thing. At its very center is the core, which
actually has two layers, the inner core and
the outer core.
The inner core is solid, and made mostly of
iron and nickel. These are heavy elements,
and sank to the center of the planet when
it was forming, leaving lighter elements like
oxygen, silicon, and nitrogen to rise to the
surface. The solid inner core is about 1200
kilometers in radius, or about 10% the radius
of the Earth.
The outer core is also mostly iron and nickel,
but it’s liquid. The material in it can
flow. It’s about 2200 kilometers thick.
The temperature in the Earth’s core is tremendously
high, reaching 5500° C. The pressure is huge
as well, as you might expect with the weight
of an entire planet sitting on top of it.
You might think at such a high temperature,
iron would be a liquid, but iron can stay
solid if the pressure is high enough. In the
inner core, the pressure is extremely high,
and even though it’s hot, iron is solid.
In the outer core, where it’s still hot,
but the pressure is a little bit lower, iron
is a liquid.
Above the core is the mantle.It’s about
2900 kilometers thick. The consistency of
the mantle is weird; most people think it’s
like lava, but really it’s like very thick
hot plastic. It behaves more or less like
a solid, but over long periods of time, geologic
periods of time, it can flow. We’ll get
back to that in a sec.
On top of the mantle is the crust, a solid
layer of rock. The overall density of the
rock in the crust is less than in the mantle,
so in a sense it floats on the mantle. There
are two types of crust on Earth: Oceanic crust,
which is about 5 kilometers thick, and continental
crust, which is a much beefier 30-50 kilometers thick.
Still, the crust is very thin compared to the other layers.
The crust isn’t a solid piece, though; it’s
broken up into huge plates, and these can
move. What drives the movement of these plates
is the flow of the rock in the mantle, and
that, in turn, is powered by heat.
The core of the Earth heats the bottom of
the mantle. This causes convection; the warmer
material rises. It’s not exactly a speed demon,
though: The rate of flow is only a couple
of centimeters per year, so it takes about 50 or 60
thousand years for a blob to move a single kilometer.
The hot material rises toward the surface,
but it’s blocked by the crust. The magmatic
rock pushes on the plates, causing them to
slide around very slowly. Your fingernails
grow at about the same rate the continents
move. Over millions of years, though, this
adds up, changing the surface geography of
the Earth—where you see continents now is
not at all where they were millions of years ago.
In some places, generally where the plates come
together, the crust is weaker. Magma can push
its way through, erupting onto the surface,
forming volcanoes. Other volcanoes, like Hawaii
or the Canary Islands, are thought to be from
a plume of hotter material punching its way
right through the middle of a continental
plate. As the plate moves, the hot spot forms
a linear chain of volcanoes over millions
of years.
Volcanoes create new land as material wells
out, but they also pump gas out of the Earth
too. A large part of Earth’s atmosphere
was supplied from volcanoes!
The interior of the Earth is hot; in the core,
it’s about as hot as the surface of the
Sun! Where did that heat come from?
Most of it is leftover from the Earth’s
formation, more than 4.5 billion years ago.
As rock and other junk accumulated to form
the proto-Earth, their collisions heated them
up. As the Earth grew that heat built up,
and it’s still toasty inside even today.
Also, as the Earth formed and gained mass
it began to contract under its own gravity,
and this squeezing added heat to the material.
Another source is elements like uranium deep
inside the Earth, which add heat as the atoms
radioactively decay. And a fourth source of
heat is from dense material like iron and
nickel sinking to the center of the Earth,
which warms things up due to friction.
All of these things add up to a lot of heat,
which is why, after all these billions of
years, the Earth still has a fiery heart.
The outer core of the Earth is liquid metal,
which conducts electricity. The liquid convects,
and this motion generates magnetic fields,
similar to the way plasma in the Sun generates
magnetic fields. The Earth’s rotation helps
organize this motion into huge cylindrical
rolls that align with the Earth’s axis.
The overall effect generates a magnetic field
similar to a bar magnet, with a magnetic north
pole and south pole, which lie close to the
physical spin axis poles of the Earth.
The loops of magnetism surround the Earth,
and play a very important role: They deflect
most of the charged particles from the solar
wind, and they trap some, too. Without the
geomagnetic field, that solar wind would hit
the Earth’s atmosphere directly. Over billions
of years, that would erode the Earth’s air
away, like a sand blaster stripping paint
off a wall. Mars, for example, doesn’t have
a strong magnetic field, and we think that’s
why its atmosphere is mostly gone today.
But we do have an atmosphere, and it’s more
than just air blowing around. Earth’s atmosphere
is the layer of gas above the crust. Because
it’s not solid, it doesn’t just stop,
it just sort of fades away with height. By accepted
definition—and by that I mean it’s not
really science, it’s more of a “Eh, let’s
just do it this way” kind of thing—the
line between Earth’s atmosphere and space
is set at 100 kilometers up. This is what’s
called the Kármán line, and if you get above
it, congratulations! You’re an astronaut.
The atmosphere is, by volume, about 78% nitrogen,
21% oxygen, 1% argon of all things, and then
an assortment of trace gases. There’s water
vapor, too, almost all of it below a height
of about 8-15 kilometers. This part of the
atmosphere is warmest at the bottom, which
means we get convection in the air, creating
currents of rising air, which carry water
with them, forming clouds, which in turn is
why we have weather.
At a height of about 25 kilometers on average
is a layer of ozone, a molecule of oxygen
that’s good at absorbing solar ultraviolet
light. That kind of light can break apart
biological molecules, so the ozone
layer is critical for our protection.
Incidentally, the Earth’s magnetic field
does more than trap solar wind particles;
it also channels some of them down into the
atmosphere, where they slam into air molecules
about 150 kilometers up. This energizes the
molecules, which respond by emitting light
in different colors: Nitrogen glows red and
blue, oxygen red and green. We call this glow
the aurora, and it happens near the geomagnetic
poles—far north and south. The lights can
form amazing ribbons and sheets, depending
on the shape of the magnetic field.
I’ve never seen an aurora. Some day.
You may not be aware of the atmosphere unless
the wind is blowing, but it’s there. It
exerts a pressure on the surface of the Earth
of about a kilogram per square centimeter,
or nearly ten tons per cubic meter! There’s
roughly ton of air pushing down on you right
now! You don’t feel it because it’s actually
pushing in all directions—down, to the sides,
even up—and our bodies have an internal
pressure that balances that out.
The Earth also has liquid water on its surface,
unique among the planets. The continental
crust is higher than oceanic crust, so water
flows down to fill those huge basins. The
Earth’s surface is about 70% covered in
water. Most likely, some of this water formed
when the Earth itself formed, and some may
have come from comet and asteroid impacts
billions of years ago. The exact proportion
of locally sourced versus extraterrestrial
water is still a topic of argument among scientists.
Earlier, I mentioned trace molecules of gas
in the atmosphere. One of these is carbon
dioxide, which only constitutes about 0.04%
of the lower atmosphere. But it’s critical.
Sunlight heats the ground, which emits infrared
light. If this infrared light were allowed
to radiate into space, the Earth would cool.
But carbon dioxide traps that kind of light,
and the Earth doesn’t cool as efficiently.
This so-called greenhouse effect warms the
Earth. Without it, the average temperature
on Earth would be below the freezing point
of water! We’d be an iceball.
This is why climate scientists are concerned
about carbon dioxide. A little is a good thing,
but too much can be very dangerous. Since
the Industrial Revolution, we’ve added a
lot of the gas to our atmosphere, trapping
more heat. By every measure available, the
heat content of the Earth is increasing, upsetting
the balance. It’s melting glaciers in Antarctica
and Greenland, as well as sea ice at the north
pole. Sea levels are going up, and some of
the extra CO2 in the air is absorbed by the
oceans, acidifiying them.
There's an old concept in science fiction called
terraforming: Going to uninhabitable alien
planet and engineering it to be more Earthlike.
I don’t know what the opposite process would
be called, but it’s what we’re doing to
Earth right now.
The Earth is the only habitable planet in
the solar system. And you know what?
We should  keep it that way.
Today you learned that the Earth is a planet,
with a hot core, a thick layer of molten rock
called the mantle, and a thin crust. The outer
core generates a strong magnetic field, which
protects the Earth’s atmosphere from the
onslaught of the solar wind. Motion in the
mantle creates volcanoes, and the surface
is mostly covered in water. The Earth’s
atmosphere is mostly nitrogen, and it’s
getting warmer due to human influence.
Crash Course is produced in association with PBS
Digital Studios. This episode was written by me,
Phil Plait. The script was edited by Blake de Pastino,
and our consultant is Dr. Michelle Thaller. It was
co-directed by Nicholas Jenkins and Michael Aranda,
and the graphics team is Thought Café.