What Planets Have Surface Features and What Are They?

Every rocky and icy world in our solar system carries a record of its history on its surface, from impact craters and volcanic plains to canyon systems and glacial ice sheets. The planets with true solid surfaces you can map and study are Mercury, Venus, Earth, and Mars. Gas and ice giants like Jupiter, Saturn, Uranus, and Neptune have no solid ground at all. But the story extends well beyond the four terrestrial planets: dwarf planets like Ceres and Pluto, and dozens of moons, also host remarkable and sometimes bizarre surface geology.

Mercury’s Battered, Shrunken Crust

Mercury is the smallest planet and the closest to the Sun, and its surface reads like a logbook of billions of years of bombardment and internal cooling. The landscape is dominated by impact craters of every size, from small pits to enormous basins. The Caloris basin, one of the largest impact structures in the solar system, stretches roughly 1,550 kilometers across and anchors much of Mercury’s geological story. High-resolution images from NASA’s MESSENGER spacecraft revealed volcanic vents around the basin’s inner margin and showed that plains of lava were laid down sequentially inside and around numerous large craters, sometimes to thicknesses of several kilometers.¹

Volcanism, in fact, shaped a surprisingly large portion of Mercury. About 27% of the planet’s surface is covered by smooth plains produced mainly by extensive flood-style lava eruptions.² Within those smooth plains, researchers have identified several hundred “ghost craters,” impact features that were nearly or completely buried by lava flows and are now visible only as faint rings of deformational ridges and wrinkles on the surface.³ Mercury also has enormous scarps, cliff-like features hundreds of kilometers long, that formed as the planet’s interior cooled and the whole world shrank slightly, compressing the crust.

Venus Behind the Clouds

Venus is Earth’s near-twin in size, but its surface is hidden beneath a thick atmosphere of carbon dioxide and sulfuric-acid clouds. Everything we know about its terrain comes from radar, most of it from NASA’s Magellan spacecraft in the early 1990s. Magellan’s synthetic aperture radar imaged most of Venus at a resolution better than 300 meters and mapped topography to a vertical accuracy better than 50 meters.⁴ What it revealed was a world shaped overwhelmingly by volcanism and tectonic deformation, with relatively few impact craters compared to Mercury or the Moon.

One of Venus’s most distinctive terrain types is tessera, a heavily deformed surface crisscrossed by multiple sets of ridges and fractures. Tessera terrain contains the oldest rocks preserved on Venus’s surface, making it a key target for understanding the planet’s early history.⁵ Some tessera, however, may have formed more recently through deformation of younger volcanic plains, complicating the picture.⁶ Beyond tessera, Venus hosts thousands of volcanic structures including shield volcanoes, lava channels stretching thousands of kilometers, and distinctive flat-topped “pancake” domes found nowhere else in the solar system. Coronae, large circular features surrounded by concentric ridges and troughs, are thought to form where hot plumes of mantle material push up from below.

ESA’s planned EnVision mission aims to dramatically sharpen our view of Venus, carrying a radar system capable of imaging selected areas at resolutions as fine as one meter and detecting centimeter-scale surface changes through repeat observations. That would allow scientists to determine whether Venus is geologically active right now, something Magellan’s single mapping pass could not settle.⁷

Earth as a Planetary Surface

Earth is the planet whose surface features you know best, but it is worth stepping back and seeing it the way a planetary scientist would. Earth is the only planet with an active hydrological cycle involving liquid water, which gives it surface processes found nowhere else: river erosion that carves valleys and builds deltas, glaciers that grind down mountain ranges, ocean waves that reshape coastlines, and sedimentary basins that accumulate and compact material over hundreds of millions of years. These water-driven processes are so efficient at erasing older features that impact craters, which dominate the faces of Mercury and the Moon, are rare and faint on Earth’s surface.

Earth also has plate tectonics, the continuous recycling of the crust through subduction and spreading. No other planet in our solar system has been confirmed to operate this way. Plate tectonics builds mountain ranges where plates collide, opens ocean basins where they spread apart, and drives volcanism at plate boundaries and hotspots. The result is a surface that is geologically young and constantly renewed, with an average ocean-floor age of only about 80 million years, a blink compared to the 4-billion-year-old surfaces common on Mercury and Mars.

Mars and Its Record of Lost Water

Mars has arguably the most dramatic single surface features of any planet. Olympus Mons, the tallest volcano in the solar system, rises roughly 22 kilometers above the surrounding terrain. It sits within the Tharsis Volcanic Province, which covers about a quarter of the Martian surface and hosts over a thousand identified small volcanic vents formed from distributed eruptions across the region.⁸ Volcanism on Mars was active for an extraordinarily long time, spanning more than 3.5 billion years, but gradually became concentrated in the Tharsis region, where the most recent eruptions occurred as recently as 100 to 200 million years ago.⁹

Valles Marineris, the great canyon system stretching over 4,000 kilometers along Mars’s equator, is often compared to Arizona’s Grand Canyon but is an order of magnitude larger. It is not a water-carved canyon. Structural analysis shows that key sections like Coprates Chasma formed as grabens, blocks of crust dropped down between parallel faults, driven by tectonic stresses associated with the Tharsis volcanic region.¹⁰ The overall structure resembles a wide rift system, with modeling suggesting that a combination of crustal thickness and heat flow governed whether the troughs formed as wide or narrow rifts.¹¹

Water, though, left its own deep mark on Mars. In Gale crater, the Curiosity rover found layered sedimentary rocks interpreted as evidence of ancient streams, deltas, and a lake that existed intermittently for thousands to millions of years, implying a climate wet enough to deliver sustained runoff.¹² In Jezero crater, the Perseverance rover found inclined strata consistent with deltas that advanced into a standing lake, topped by boulder conglomerates deposited by high-energy floods, recording a shift from a long-lived lake environment to brief, violent flood events.¹³ Orbital images in the Nili Fossae region have also revealed two valley networks feeding distributary fans into an ancient 40-kilometer-wide crater lake that ponded to about 450 meters deep before overtopping its rim.¹⁴ Collectively, these findings paint a picture of a planet where liquid water once flowed on the surface long enough to build the kinds of sedimentary deposits we associate with habitable environments on Earth.

Why Gas Giants Do Not Qualify

Jupiter, Saturn, Uranus, and Neptune are often called gas giants (or, for Uranus and Neptune, ice giants), and their defining trait for this question is straightforward: they do not have solid surfaces. Their atmospheres are dominated by hydrogen and helium, and as you descend through increasingly dense cloud layers, the gas transitions smoothly into liquid and eventually into exotic high-pressure states without ever hitting a ground you could stand on.¹⁵ They have atmospheric features, of course, including Jupiter’s Great Red Spot, Saturn’s hexagonal polar vortex, and Neptune’s transient dark spots. But these are weather patterns in fluid envelopes, not surface geology.

That said, the moons orbiting these giant planets are some of the most geologically interesting objects in the solar system. Many have solid, icy surfaces with genuine geology, and a few are discussed below.

Dwarf Planets and Small Icy Worlds

Ceres, the largest object in the asteroid belt and a dwarf planet, surprised scientists when NASA’s Dawn spacecraft arrived in 2015. Its surface is not just a passive collection of impact craters. Analysis of Dawn’s images showed that Ceres has experienced cryovolcanism, the extrusion of icy material from depth, throughout its geological history, at an average rate of roughly 10,000 cubic meters per year.¹⁶ The most visible result is Ahuna Mons, a dome-shaped mountain about 4 kilometers high that appears to be a cryovolcanic construct, a mountain built by salty, muddy ice oozing up from the interior rather than by molten rock.

Pluto, visited by New Horizons in 2015, turned out to have one of the most visually striking surfaces in the solar system. Sputnik Planitia, the left lobe of the heart-shaped Tombaugh Regio, is a vast basin filled with nitrogen ice that displays a highly diverse range of terrains, including convection cells where warmer nitrogen wells up from below and cooler nitrogen sinks. Rugged water-ice mountains surround the basin, including peaks informally named Hillary Montes and Tenzing Montes, shaped over time by glacial flow. Further east, “bladed terrain” deposits of methane ice rise like knife-edge ridges, and nitrogen ice patches fill depressions and crater floors.¹⁷ Pluto’s surface is actively reworked by cycles of nitrogen and methane sublimation and deposition, making it far more dynamic than anyone expected of a small, cold world at the edge of the solar system.

Moons Worth Mentioning

Several moons have surface geology as interesting as any planet’s. Io, Jupiter’s innermost large moon, is the most volcanically active body known. Tidal forces from Jupiter continuously flex Io’s interior, generating enough heat to drive hundreds of active volcanic centers. Modeling suggests that asymmetric melting patterns in Io’s interior shift the peak zone of tidal heating away from the point directly facing Jupiter, which promotes volcanism and outgassing in particular regions, a feedback mechanism also expected to operate on tidally heated exoplanets and exomoons.¹⁸ The result is a surface constantly being paved over by fresh lava flows and sulfurous deposits, with virtually no impact craters surviving.

Titan, Saturn’s largest moon, is the only moon with a dense atmosphere and the only world besides Earth known to have stable liquid on its surface right now. But Titan’s lakes and seas are filled with liquid methane and ethane, not water. Its equatorial regions are covered by vast fields of hydrocarbon sand dunes. NASA’s upcoming Dragonfly mission is a rotorcraft lander designed to hop across Titan’s surface, sampling organic sediments in the dune fields and water ice in interdune areas, ultimately heading to the 80-kilometer-wide Selk crater, where liquid water from the impact may have mixed with surface organics.¹⁹ Europa and Enceladus, icy moons of Jupiter and Saturn respectively, have surfaces shaped by tectonic fracturing and possible cryovolcanic activity, with subsurface oceans lurking beneath their ice shells. Their surfaces are young and sparsely cratered, hinting at ongoing geological processes driven by tidal heating.

Sand Dunes Across the Solar System

One surface feature that turns up on multiple worlds is sand dunes, which form wherever there is loose granular material and a fluid capable of moving it. Earth, Mars, Venus, and Titan all have dune fields, but the physics differ because the atmospheres and grain compositions vary so widely. On Mars, wind simulations reproduce the wide variety of observed dune shapes, from classic crescent-shaped barchans to complex star dunes, by modeling the shifting wind directions that sculpt them.²⁰

Venus’s atmosphere is so dense that it behaves more like a fluid than a gas at the surface, and numerical modeling shows that this environment can generate small barchan dunes similar to those formed underwater on Earth, though they develop more slowly.²¹ Across all these worlds, the size of dunes that first form when wind disturbs a flat sand bed scales with a drag length that depends on grain size, grain density, and the density and viscosity of the surrounding fluid. This relationship holds from tiny underwater ripples on Earth to massive Martian dune fields, providing a single physical framework that links dune formation across very different planetary environments.²²

How Surfaces Age Without Air or Water

On bodies with no atmosphere and no liquid water, surfaces still change, just through different processes. Space weathering refers to the slow alteration of exposed rock and soil by solar wind particles, micrometeorite impacts, and cosmic rays. On the Moon, this has been studied in detail using returned samples. Lunar soil accumulates tiny opaque particles, including nanoscale metallic iron, on the surfaces and interiors of individual grains. These particles change how the soil reflects light: the finest iron particles redden the visible and near-infrared spectrum, while larger particles darken it across all wavelengths.²³ The effect matters practically because planetary scientists use surface color and brightness to infer composition from orbit. A space-weathered surface can look chemically different from a fresh one made of the same rock, which has to be accounted for when mapping the geology of Mercury, asteroids, and other airless bodies.

Impact cratering is the other universal process. On any solid surface in the solar system, counting craters and measuring their sizes is the primary method for estimating how old a surface is. A region with many craters per unit area is older; a region with few is younger, resurfaced by lava, ice, or tectonic activity at some point.²⁴ The technique has limits, especially on small areas where random variation in crater counts introduces large uncertainties, but it remains the backbone of planetary chronology for every world we cannot sample directly.²⁵

Searching for Surface Clues on Distant Worlds

All the surface features discussed so far belong to worlds we have visited with spacecraft or studied with powerful telescopes at relatively close range. For planets orbiting other stars, detecting surface features is far beyond current capability, but researchers are already developing the methods that might someday make it possible. One approach involves watching how the brightness of a planet changes as it orbits its star, passing through different illumination phases much as the Moon does from our perspective. Spectral unmixing experiments modeling an Earth-like exoplanet showed that one surface type became roughly 16 times brighter as the planet moved from a quarter-lit to a crescent phase, a signature consistent with ocean glint, the specular reflection of starlight off liquid water. A second surface type barely changed in brightness, consistent with dry land.²⁶ The technique is far from ready for real detections with current telescopes, but it illustrates a path toward eventually distinguishing oceans from continents on a world tens of light-years away. Tidal heating, the same mechanism that drives Io’s volcanism, is also expected to affect rocky exoplanets and exomoons in close orbits, potentially creating volcanic surfaces and outgassing signatures detectable through future atmospheric observations.¹⁸