Here are 10 of the coolest, weirdest and most unexpected findings about the Pluto system scientists have learned thanks to the New Horizons spacecraft’s flyby of the distant world in 2015.

Enhanced color global view of Pluto, taken when NASA’s New Horizons spacecraft was 280,000 miles (450,000 km) away. The image shows Pluto’s famous heart, a region known as Tombaugh Regio. It was recently announced that Pluto’s icy heart makes winds blow across the dwarf planet’s surface.

Image via NASA/ Johns Hopkins APL/ Southwest Research Institute)

NASA originally published this article on July 14, 2020.

On July 14, 2015, after a voyage of nearly 10 years and more than 3 billion miles, NASA’s New Horizons spacecraft flew within 7,800 miles (12,550 km) of Pluto. Thanks to the piano-sized probe, we saw the surface of this distant world in spectacular, colored detail for the first time.

The encounter – which also included a detailed look at Charon, the largest of Pluto’s five moons – revealed an icy world replete in magnificent landscapes and geology, with towering mountains, giant ice sheets, pits, scarps, valleys and terrains seen nowhere else in the solar system.

In the five years since that groundbreaking flyby, nearly every conjecture about Pluto being an inert ball of ice has been thrown out the window.

Here are 10 of the coolest, weirdest and most unexpected findings about the Pluto system that scientists have learned since 2015, thanks to data from New Horizons.

Natural-color view of Pluto and its large moon Charon, compiled from images taken by NASA’s New Horizons spacecraft on July 13 and 14, 2015. Of all the moon-planet systems in our solar system, Pluto and Charon are most nearly alike in size. Charon is nearly half the size of Pluto. It’s so big relative to Pluto that the 2 worlds are sometimes considered a double dwarf planet.

Image via NASA/ Johns Hopkins APL/ Southwest Research Institute.

1. Pluto has a “heart,” and it drives activity on the planet

Pluto’s heart – one of the signature features New Horizons observed on approach and imaged in high resolution during the flyby – is a vast, million-square-mile nitrogen glacier. The heart’s left ventricle, called Sputnik Planitia, literally forced the dwarf planet to reorient itself so the basin now faces almost squarely opposite Pluto’s moon Charon.

James Tuttle Keane is a planetary scientist and New Horizons team member at the Jet Propulsion Laboratory in Pasadena, California. He said:

It’s a process called true polar wander – it’s when a planetary body changes its spin axis, usually in response to large geologic processes.

Sputnik Planitia’s current position is no accident. It’s a cold trap, where nitrogen ices have accumulated to make an ice sheet that’s at least 2.5 miles (4 kilometers) thick. The constant imbalance of that hefty mass, combined with the tidal yanks and pulls of Charon as it orbited Pluto, literally tipped the dwarf planet so the basin aligned more closely with the tidal axis between Pluto and Charon. Keane said:

That event was also likely responsible for cracking Pluto’s surface and creating the many gigantic faults in its crust that zigzag over large portions of Pluto.

The basin is thought to have formed to the northwest of its present location, and closer to Pluto’s north pole. And should ices continue to accumulate on the basin, Pluto will continue to reorient itself.

Cross-section of Pluto’s surface and subsurface features, in the region of Sputnik Planitia, the western lobe of Pluto’s heart. New Horizons data suggest there may be a water ocean beneath the ice in this region.

Image via James Tuttle Keane/ NASA.

2. There’s probably a vast liquid water ocean sloshing beneath Pluto’s surface

Gathered ices may not be the only thing that helped reorient Sputnik Planitia. New Horizons data from the basin indicated there may be a heavier mass beneath it that played a part, and scientists suspect that the heavier mass is a water ocean. Keane said:

That was an astonishing discovery. It would make Pluto an elusive ‘ocean world,’ in the same vein as Europa, Enceladus and Titan.

Several other lines of evidence, including tectonic structures seen in New Horizons imagery, also point to an ocean beneath Pluto’s crust.

Sputnik Planitia was likely created some 4 billion years ago by the impact of a Kuiper Belt object 30 to 60 miles (50 to 100 km) across that carved out a massive chunk of Pluto’s icy crust and left only a thin, weak layer at the basin’s floor. A subsurface ocean likely intruded the basin from below by pushing up against the weakened crust, and later the thick layer of nitrogen ice seen there now was laid on top.

Recent models based on images of the planet suggest that this liquid ocean may have arisen from a rapid, violent formation of Pluto.

The subsurface ocean on Pluto may be still in the process of freezing and potentially creating new faults on the surface today.

Image via James Tuttle Keane/ NASA.

3. Pluto may still be tectonically active because that ocean is still liquid

Enormous faults stretch for hundreds of miles and cut roughly 2.5 miles into the icy crust covering Pluto’s surface. One of the only ways scientists reason Pluto got those fissures, though, is by the gradual freezing of an ocean beneath its surface.

Water expands as it freezes, and under an icy crust, that expansion will push and crack the surface, just like an ice cube in your freezer. But if the temperature is low enough and the pressure high enough, water crystals can start to form a more compact crystal configuration and the ice will once again contract.

Models using New Horizons data showed Pluto has the conditions for that type of contraction, but it doesn’t have any known geologic features that indicate that contraction has occurred. To scientists, that means the subsurface ocean is still in the process of freezing and potentially creating new faults on the surface today. Keane said:

If Pluto is an active ocean world, that suggests that the Kuiper Belt may be filled with other ocean worlds among its dwarf planets, dramatically expanding the number of potentially habitable places in our solar system.

But while Pluto’s liquid ocean likely still exists today, scientists suspect it’s isolated in most places (though not beneath Sputnik) by almost 200 miles (320 km) of ice. That means it probably doesn’t contact the surface today; but in the past, it may have oozed through volcanic activity called cryovolcanism.

Close up view of Wright Mons, one of two potential cryovolcanoes – volcanoes that spew ice instead of lava – spotted on the surface of Pluto by the passing New Horizons spacecraft in July 2015.

Image via NASA/ Johns Hopkins APL/ Southwest Research Institute.

4. Pluto was – and still may be – volcanically active

But maybe not “volcanic” in the way you might think.

On Earth, molten lava spits, drools, bubbles, and erupts from underwater fissures through volcanoes sitting miles high in and protruding from the oceans, like on Hawaii. But on Pluto, there are numerous indications that a kind of cold, slushy cryolava has poured over the surface at various points.

Scientists call that “cryovolcanism.”

Wright Mons and Piccard Mons, two large mountains to the south of Sputnik Planitia, each bear a deep central pit that scientists believe are likely to be the mouths of cryovolcanoes unlike any others found in the solar system.

To the west of Sputnik sits Viking Terra, with its long fractures and grabens that show evidence of once-flowing cryolavas all over the surface there too.

And farther west of Sputnik Planitia is the Virgil Fossae region, where ammonia-rich cryolavas seem to have burst to the surface and coated an area of several thousand square kilometers in red-colored organic molecules no more than 1 billion years ago, if not even more recently.

And speaking of recently…

You’ve seen the images of Pluto’s famous heart. This is a close-up of a region in the western lobe of the heart, a region called Sputnik Planitia. This image spans about 50 miles (80 km) and shows thousands of pits in Pluto’s icy surface as well as larger circulation patterns. Scientists suspect the “islands” are floating bergs of water ice, or perhaps the tips of ice mountains.

Image via NASA/ Johns Hopkins APL/ Southwest Research Institute.

5. Glaciers cut across Pluto’s surface even today, and they’ve done so for billions of years

Pluto joins the ranks of Earth, Mars, and a handful of moons that have actively flowing glaciers.

East of Sputnik Planitia are dozens of (mostly) nitrogen-ice glaciers that course down from pitted highlands into the basin, carving out valleys as they go. Scientists suspect seasonal and “mega-seasonal” cycles of nitrogen ices that sublimate from ice to vapor, waft around the dwarf planet and then freeze back on the surface are the source of the glacier ice.

But these glaciers are not like our own water-ice glaciers here on Earth. For one, any melt within them won’t fall toward the bottom of the glacier. It will rise to the top, because liquid nitrogen is less dense than solid nitrogen. As that liquid nitrogen emerges on top of the glacier, it potentially even erupts as jets or geysers.

Additionally, there is the fact that some of Pluto’s surface is composed of water ice, which is slightly less dense than nitrogen ice. As Pluto’s glaciers carve the surface, some of those water-ice “rocks” will rise up through the glacier and float like icebergs. Such icebergs are seen in several New Horizons images of Sputnik Planitia, the largest of Pluto’s known glaciers, which stretches more than 620 miles (1,000 km) across – about the size of Oklahoma and Texas combined.

Scientists from NASA’s New Horizons mission used state-of-the-art computer simulations to show that the surface of Pluto’s Sputnik Planitia is covered with churning ice “cells” that are geologically young and turning over due to the process of convection (same process you see in a pan of boiling water).

Image via NASA/ Johns Hopkins APL/ Southwest Research Institute.

6. Pluto has heat convection cells on its giant glacier Sputnik

Zoom in close to the surface of Sputnik Planitia and you’ll see something unlike anywhere else in the solar system: a network of strange polygonal shapes in the ice, each at least 6 miles (10 km) across, churning on the surface of the glacier.

Although they resemble cells under a microscope, these aren’t; they’re evidence of Pluto’s internal heat trying to escape from underneath the glacier, and forming bubbles of upwelling and downwelling nitrogen ice, something like a hot lava lamp.

Warm ice rises up into the center of the cells while cold ice sinks along their margins. There’s nothing like it in any of Earth’s glaciers, and or anywhere else in the solar system that we’ve explored!

White area is lobe of Pluto’s “heart,” a vast area of nitrogen ice which cycles from vapor to condensation every day, driving nitrogen winds around the planet.

Image via NASA.

7. Pluto has a literal beating “heart” that controls its atmosphere and climate

Cold and far-flung as Pluto may be, its icy “heart” still beats to a daily, rhythmic drum that drives Pluto’s atmosphere and climate much in the way Greenland and Antarctica help control Earth’s climate.

Nitrogen ices in Pluto’s heart-shaped Tombaugh Regio go through a cycle every day, subliming from ice to vapor in the daytime sunlight and condensing back on the surface during the frigid night. Each round acts like a heartbeat, driving nitrogen winds that circulate around the planet at up to 20 mph (32 kph).

Tanguy Bertrand is a planetary scientist at NASA Ames Research Center in Mountain View, California. Bertrand said:

Pluto’s heart actually controls its atmosphere circulation.

Sophisticated weather forecast models Bertrand has created using New Horizons data show that as these ices sublime in the northern reaches of Pluto’s icy heart and freeze out in the southern part, they drive brisk winds in a westward direction – curiously opposite Pluto’s eastward spin.

Those westward winds, bumping up against the rugged topography at the fringes of Pluto’s heart, explain why there are wind streaks on the western edge of Sputnik Planitia, a remarkable finding considering Pluto’s atmosphere is only 1/100,000th that of Earth’s, Bertrand said. They also explain some other surprising desert-like features …

Closeup of the water-ice mountains on the northwest fringes of Pluto’s Sputnik glacier may provide the particles, and Pluto’s beating nitrogen “heart” provides winds.

Image via NASA/ Johns Hopkins APL/ Southwest Research Institute.

8. Pluto has dunes

It’s not the Sahara Desert, or the Gobi Desert. This is Pluto. Hundreds of dunes stretch over at least 45 miles (75 km) of the western edge of Sputnik Planitia, and scientists suspect they formed recently.

Dunes require small particles and sustained, driving winds that can lift and blow the specks of sand or whatever else along. And despite its weak gravity, thin atmosphere, extreme cold and entire surface composition of ices, Pluto apparently had (or still may have) everything needed to make dunes.

Water-ice mountains on the northwest fringes of the Sputnik glacier may provide the particles, and Pluto’s beating nitrogen “heart” provides winds. Instead of quartz, basalt and gypsum sands blown by sometimes gale-force winds on Earth, though, scientists suspect the dunes on Pluto are sand-sized grains of methane ice carried by winds that blow at no more than 20 mph (32 kph), although given the size of the dunes, the winds may have been stronger and atmosphere much thicker in the past.

Pluto and Charon are dotted with large craters, but there are few small ones, possibly indicating fewer small Kuiper Belt objects than expected.

Image via NASA.

9. Pluto and Charon have almost no little craters, and that has some big implications

Finding craters on the surface of planets is kind of the norm in space. But if there’s one abnormal thing about the Pluto system, it’s that neither Pluto nor Charon has many small craters – they’re almost all big.

Kelsi Singer is a New Horizons deputy project scientist and co-investigator from the Southwest Research Institute in Boulder, Colorado. She said:

That surprised us because there were fewer small craters than we expected, which means there are also fewer small Kuiper Belt objects than we expected.

Analyses of crater images from New Horizons indicate that few objects less than about a mile in diameter bombarded either world. Because scientists have no reason to believe tectonic activity would have preferentially wiped the surface clean of these small craters, It could mean the Kuiper Belt is mostly devoid of very small objects. Singer said:

These results give us clues about how the solar system formed because they tell us about the population of building blocks of larger objects, like Pluto and even perhaps Earth.

Enhanced color view of Pluto’s largest moon, Charon. The colors are processed to highlight the variation of surface properties across the moon; most striking is the reddish north (top) polar region.

Image via NASA/ Johns Hopkins APL/ Southwest Research Institute.

10. Charon had a volcanic past, and it could be key to understanding other icy worlds

New Horizons also captured stunning images of Pluto’s moon Charon, and they revealed some surprising geology there too.

On the side of Charon that New Horizons imaged in high resolution, Charon has two distinct terrain types: an immense, southward-stretching plain officially called Vulcan Planitia that’s at least the size of California, and a rugged terrain colloquially called Oz Terra that stretches northward to Charon’s north pole. Both seem to have formed from the freezing and expansion of (you guessed it!) an ancient ocean beneath Charon’s crust.

Moderate expansion in the north created the rugged, mountainous terrain of Oz Terra seen today, whereas the expansion in the south forced its way through vents, cracks and other openings as cryolava, spilling across the surface. In fact, Vulcan Planitia is thought to be a giant cryoflow that covered the entire region early in Charon’s history.

Similar features exist on some icy satellites all around the solar system, including Neptune’s giant moon Triton, Saturn’s moons Tethys, Dione and Enceladus, and Uranus’ moons Miranda and Ariel. And thanks to the detailed images of Charon from New Horizons, the models of Charon’s past might be a Rosetta Stone to aid in understanding the volcanic and geologic activity of those other icy worlds too.

• Bottom line: Ten cool things about Pluto, from New Horizons data.
• Via NASA

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“This study significantly changes the view of Venus from a mostly inactive planet to one whose interior is still churning and can feed many active volcanoes,” one scientist said.

On Venus, ring-like structures known as coronae dot the surface of the planet. They’re thought to provide evidence of a warm interior and for ongoing geologic activity. In the global map of Venus above, the 37 coronae determined to be active in the new study appear in red, and inactive coronae appear in white.

Image via Anna Gülcher/ University of Maryland.

Researchers at the University of Maryland and the Institute of Geophysics at ETH Zurich, Switzerland, announced today (July 20, 2020) that their new new 3D model of cloud-covered Venus identifies 37 recently active volcanic structures. They said their study “provides some of the best evidence yet” that Venus is today a geologically active world. The peer-reviewed journal Nature Geoscience published these scientists’ work today. 

Laurent Montési, a professor of geology at UMD and co-author of the research paper, said:

This is the first time we are able to point to specific structures and say ‘Look, this is not an ancient volcano but one that is active today, dormant perhaps, but not dead.’ This study significantly changes the view of Venus from a mostly inactive planet to one whose interior is still churning and can feed many active volcanoes.

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A 3D rendition of 2 coronae observed on Venus’ surface. The ringlike structures are formed when hot material from deep inside Venus rises through the planet’s mantle and erupts through its crust. The black line represents a gap in the data.

Image via Laurent Montési/ University of Maryland.

A statement from University of Maryland explained:

Scientists have known for some time that Venus has a younger surface than planets like Mars and Mercury, which have cold interiors. Evidence of a warm interior and geologic activity dots the surface of the planet in the form of ring-like structures known as coronae, which form when plumes of hot material deep inside the planet rise through the mantle layer and crust. This is similar to the way mantle plumes formed the volcanic Hawaiian Islands.

But it was thought that the coronae on Venus were probably signs of ancient activity, and that Venus had cooled enough to slow geological activity in the planet’s interior and harden the crust so much that any warm material from deep inside would not be able to puncture through.

In addition, the exact processes by which mantle plumes formed coronae on Venus and the reasons for variation among coronae have been matters for debate.

In the new study, the researchers used numerical models of thermomechanical activity beneath the surface of Venus to create high-resolution, 3D simulations of coronae formation. Their simulations provide a more detailed view of the process than ever before.

The results helped Montési and his colleagues identify features that are present only in recently active coronae. The team was then able to match those features to those observed on the surface of Venus, revealing that some of the variation in coronae across the planet represents different stages of geological development.

The study provides the first evidence that coronae on Venus are still evolving, indicating that the interior of the planet is still churning.

Anna Gülcher is a Ph.D. student in the Geophysical Fluid Dynamics group at ETH Zürich and lead author of the new study.

Montési added:

The improved degree of realism in these models over previous studies makes it possible to identify several stages in corona evolution and define diagnostic geological features present only at currently active coronae. We are able to tell that at least 37 coronae have been very recently active.

The active coronae on Venus are clustered in a handful of locations, which suggests areas where the planet is most active, providing clues to the workings of the planet’s interior. These results may help identify target areas where geologic instruments should be placed on future missions to Venus, such as Europe’s EnVision mission, scheduled to launch in 2032.

We’ve known about volcanic mountains on Venus for some time. Here is Maat Mons, a massive Venusian shield volcano. It’s the second-highest mountain – and the highest volcano – on Venus, rising some 5 miles (8 km) high. This perspective view is based on radar images from the Magellan spacecraft, which orbited Venus from 1990 to 1994. Maat Mons is not one of the locations evaluated in the new study, by the way. This structure on Venus be inactive or active, but the new study doesn’t address that question. In addition, there could be additional locations of current activity on Venus not pinpointed by the new study.

Image via NASA Photo Journal.

• Bottom line: A new 3D model of cloud-covered Venus provides evidence that this neighboring planet has active volcanoes.
• Source: Corona structures driven by plume-lithosphere interactions and evidence for ongoing plume activity on Venus
• Via University of Maryland

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