Astro Update: The Ocean Beneath Pluto’s Wandering Heart

 A close-up high-resolution image of Pluto’s surface. By NASA/JHUAPL/SWRI

A close-up high-resolution image of Pluto’s surface. By NASA/JHUAPL/SWRI

Speculation about what lies beneath Pluto’s icy surface began long before the New Horizons spacecraft flew by the dwarf planet in September, 2015. Before the flyby, the odds that Pluto once had a subsurface ocean seemed high. Now, it seems more likely than not that some amount of liquid may still be lurking beneath the Kuiper-belt-object’s frozen crust.

Pluto and Chiron. From NASA/Johns Hopkins University Applied Physics Laboratory/Southwest Research Institute.

Pluto and Chiron. From NASA/Johns Hopkins University Applied Physics Laboratory/Southwest Research Institute.

Pluto is a comparatively small body with a comparatively enormous primary moon. Not only is Chiron half the size and one-eighth the mass of Pluto, but it is very close to the dwarf-planet’s surface: twenty times closer than our own Moon is to Earth. Given the strength of the tides on Earth, it seemed reasonable that Chiron would be strongly pulling on Pluto, heating the inside of the dwarf planet from the inside out, melting volatiles – materials like water that can be separated from rock with heating – which can then form into oceans.

The best current evidence that we have for Pluto’s possible ocean comes from Pluto’s wandering heart: a large geologic feature that looks a bit like Earth’s first artificial satellite, Sputnik. Sputnik Planum, as it’s come to be called, seems to have been made when a large object struck Pluto near its north pole. A paper published on November 16th, 2016 points out that the crater should have remained a heart-shaped hole in the ground, with less mass than when it started. Instead, Sputnik Planum grew and grew, so much so that it actually caused Pluto’s access to tilt. Models of how this might be possible call for a substantial amount of water under a crust of frozen nitrogen.

Theoretical structure of Pluto Frozen nitrogen Water ice Rock. From NASA / Johns Hopkins University Applied Physics Laboratory / Southwest Research Institute.

Theoretical structure of Pluto Frozen nitrogen Water ice Rock. From NASA / Johns Hopkins University Applied Physics Laboratory / Southwest Research Institute.

These days, Pluto’s heart lies closer to the equator than it does to the pole. Though the studies will continue, in the end, we may have an ocean to thank for that.

Courtesy of NASA.

Courtesy of NASA.

 

 


More than Only Skin Deep – What Waits Beneath Charon’s Cracked Surface

By Sheyna Gifford (originally posted June 24, 2014)

An artist’s concept of Pluto as viewed from the surface of one its moons. Pluto is the large disk at the center of the image. Charon is the smaller disk to the right. Image Credit: NASA, ESA and G. Bacon (STScI)

An artist’s concept of Pluto as viewed from the surface of one its moons. Pluto is the large disk at the center of the image. Charon is the smaller disk to the right. Image Credit: NASA, ESA and G. Bacon (STScI)

Is there evidence of an ocean-past or present-waiting to surprise us on Charon? It isn’t impossible. In fact, it might be likely.

What used to be the smallest planet in our solar system has, comparatively, the biggest moon. Pluto, now classified as a dwarf planet, has a moon, Charon, almost 1/8th its own mass and almost half its physical volume.  Our Moon, by comparison, has about 1% of the Earth’s mass and only 2% of its volume. Charon is so large compared to Pluto that some astronomer’s consider the two to be a sort of binary dwarf-planet system, as opposed to a moon-and-planet system.

Both Charon and our Moon are believed to have formed in the same way: when they were knocked off their parent planets. Enormous collisions liquified parts of the Earth and Pluto. The debris was thrown into orbit where it later cooled. In the process of cooling into solid bodies around the Earth and Pluto, the Moon and Charon became locked to their parent planets’ orbits. That locking of the planets to moons results in tides: here on Earth, on the Moon, and, we believe, on Pluto and Charon.

An analysis by scientists at Goddard suggests that tides on Pluto and Charon could have been especially high as Charon cooled. This is because the part of Pluto knocked into orbit didn’t get very far. Charon formed incredibly close to Pluto: only 19,000 km (12,000 miles) away. By comparison, our Moon is currently 384,000 km (238,855 mi) from Earth. Initially, the orbit might not have been very circular, either: it might have been more eccentric or elliptical-shaped. Eccentrically-moving, close-by Charon would have pulled on Pluto, and Pluto would have pulled back, resulting in heating of both planets and–maybe–an ocean under Charon’s ice shell.

Artist impression of the New Horizons spacecraft as it approached Jupiter en route to Pluto. Credit: NASA

Artist impression of the New Horizons spacecraft as it approached Jupiter en route to Pluto. Credit: NASA

“Depending on exactly how Charon’s orbit evolved, particularly if it went through a high-eccentricity phase, there may have been enough heat from tidal deformation to maintain liquid water beneath the surface of Charon for some time,” said Alyssa Rhoden of NASA’s Goddard Space Flight Center in Greenbelt, Maryland. “Using plausible interior structure models that include an ocean, we found it wouldn’t have taken much eccentricity (less than 0.01) to generate surface fractures like we are seeing on Europa.”

On icy moons like Europa and Enceladus, tidal forces exerted by their parent planets cause massive surface cracks to form. Those cracks are easily appreciated by passing spacecraft. According to Rhoden and colleagues’ model, Charon’s surface should be similarly cracked. We expect to see evidence of this fractured surface geology as the New Horizons spacecraft approaches Pluto. New Horizons will pass directly over Pluto and Charon, briefly, on July 15th 2015.

Charon was discovered thirty-five years ago, in 1978, but well-photographed for the first time by New Horizons in 2013. With the 2015 close-up just around the corner, scientists are working swiftly to make best use of surface photographs returned by the spacecraft. New Horizons will give us the ability to resolve objects as small as a football field on part of the surface of Pluto and Charon. With pictures of that detail and models such as this one, we may be able to look backwards in time to determine details about both bodies, such as how thick their ice shells were when they formed.

Studying patterns of fractures in Charon’s surface is critical to building accurate models of the ice shell and layers beneath.

“Our model predicts different fracture patterns on the surface of Charon depending on the thickness of its surface ice, the structure of the moon’s interior and how easily it deforms, and how its orbit evolved,” said Rhoden. “By comparing the actual New Horizons observations of Charon to the various predictions, we can see what fits best and discover if Charon could have had a subsurface ocean in its past, driven by high eccentricity.”

New Horizons LOng Range Reconnaissance Imager (LORRI) composite image showing the detection of Pluto’s largest moon, Charon. When these images were taken on July 1 and July 3, 2013, the New Horizons spacecraft was still about 550 million miles (880 million kilometers) from Pluto. On July 14, 2015, the spacecraft is scheduled to pass just 7,750 miles (12,500 kilometers) above Pluto’s surface, where LORRI will be able to spot features about the size of a football field. Credit: NASA/Johns Hopkins University Applied Physics Laboratory/Southwest Research Institute

New Horizons LOng Range Reconnaissance Imager (LORRI) composite image showing the detection of Pluto’s largest moon, Charon. When these images were taken on July 1 and July 3, 2013, the New Horizons spacecraft was still about 550 million miles (880 million kilometers) from Pluto. On July 14, 2015, the spacecraft is scheduled to pass just 7,750 miles (12,500 kilometers) above Pluto’s surface, where LORRI will be able to spot features about the size of a football field. Credit: NASA/Johns Hopkins University Applied Physics Laboratory/Southwest Research Institute

The oceans of certain icy moons with surface fractures are considered to be places where extraterrestrial life might be found. Like Charon, Europa and Enceladus are very cold and very distant from the sun. In all three cases, the formation and maintenance of life would depend upon a reliable energy source as well as elements that can participate in the chemistry of life, such as carbon, nitrogen, and phosphorus.

It is unknown if a potential ocean on Charon may have harbored these ingredients or if the ocean there existed for long enough for life to form. The same questions apply to any ancient ocean on any moon in our Solar System or any other. The first step on Charon is to find the fractures, and then go looking for the warmth that liquified water.

“Since it’s so easy to get fractures, if we get to Charon and there are none, it puts a very strong constraint on how high the eccentricity could have been and how warm the interior ever could have been,” said Rhoden. “This research gives us a head start on the New Horizons arrival – what should we look for and what can we learn from it. We’re going to Pluto and Pluto is fascinating, but Charon is also going to be fascinating.”