Examine planetary data

The planets of the Solar System show a wide range of interior structures, shaped by their size, composition, and thermal history. Based on spacecraft data, seismic studies (for Earth), gravitational measurements, and models, here is what we know:

Terrestrial Planets (Rocky)

Planet	Core	Mantle	Crust	Heat Sources	Activity Level
Mercury	Large iron-rich core (∼85% of radius), partly liquid	Thin silicate mantle	Very thin crust	Initial accretion, some radioactive decay	Geologically inactive, ancient surface
Venus	Iron-nickel core (possibly liquid)	Thick silicate mantle	Volcanic crust	Radioactive decay	Still volcanically active, no plate tectonics
Earth	Solid inner core + liquid outer core	Convecting mantle	Oceanic & continental crust	Accretion, radioactive decay	Active tectonics, strong magnetic field
Mars	Large core (partly molten), mostly iron + sulfur	Stagnant mantle	Thick basaltic crust	Some radioactive heat	Geologically dead, but once active

Gas Giants (Jupiter & Saturn)

Planet	Core	Interior Layers	Heat Sources	Activity Level
Jupiter	Possibly a rocky/icy core (~10 Earth masses)	Metallic hydrogen layer + molecular hydrogen envelope	Accretional heat + slow contraction (Kelvin–Helmholtz mechanism)	Strong magnetic field, internal heat flux
Saturn	Small dense core	Similar to Jupiter, but less massive	Accretional + gravitational settling of helium	Emits more heat than it receives from the Sun

Ice Giants (Uranus & Neptune)

Planet	Core	Mantle (Ices)	Atmosphere	Heat Sources	Activity Level
Uranus	Rocky core	Water, ammonia, methane ices	Thin hydrogen–helium atmosphere	Low internal heat	Coldest planet, minimal activity
Neptune	Similar to Uranus, but possibly larger core	“Icy” mantle of volatiles	Similar atmosphere	More internal heat than Uranus	Strong winds, dynamic weather

Dwarf Planets (e.g., Pluto)

Pluto likely has a rocky core and icy mantle.
May have or had a subsurface ocean.
Internal heating likely from radioactive decay.

Key Themes

Size matters: Larger planets retain heat longer and remain geologically active.
Composition matters: Rocky vs. gaseous vs. icy materials behave differently under pressure.
Heat sources: Gravitational accretion, radioactive decay, and slow contraction all contribute.
Magnetic fields: Produced by molten, convecting conductive layers (e.g., Earth’s outer core, Jupiter’s metallic hydrogen).

Final Note

The deeper interiors of many planets are still uncertain due to lack of direct data. Future missions (like seismometers on Mars or orbiters around Uranus/Neptune) may refine our understanding further.

Abekta

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