Category Archives: Space Science

Cassini: Magnetic anomaly leads to an ocean world circling Saturn

Saturn’s little moon Enceladus has turned out to be one of the most interesting objects in the solar system:

Cassini: Mission to Saturn: An Ice World…With an Ocean?
How a puzzling sensor reading transformed NASA’s
Cassini Saturn mission and created a new target in the search
for habitable worlds beyond Earth.

On Feb. 17, 2005, NASA’s Cassini spacecraft was making the first-ever close pass over Saturn’s moon Enceladus as it worked through its detailed survey of the planet’s icy satellites. Exciting, to be sure, just for the thrill of exploration. But then Cassini’s magnetometer instrument noticed something odd.

Since NASA’s two Voyager spacecraft made their distant flybys of Enceladus about 20 years prior, scientists had anticipated the little moon would be an interesting place to visit with Cassini. Enceladus is bright white — the most reflective object in the solar system, in fact — and it orbits in the middle of a faint ring of dust-sized ice particles known as Saturn’s E ring. Scientists speculated ice dust was being kicked off its surface somehow. But they presumed it would be, essentially, a dead, airless ball of ice.

What Cassini saw didn’t look like a frozen, airless body. Instead, it looked something like a comet that was actively emitting gas. The magnetometer detected that Saturn’s magnetic field, which envelops Enceladus, was perturbed above the moon’s south pole in a way that didn’t make sense for an inactive world. Could it be that the moon was actively replenishing gases it was breathing into space?

Thus began a hunt for clues that has turned out to be Cassini’s most riveting detective story.

“Enceladus was so exciting that, instead of just three close flybys planned for our four-year primary mission, we added 20 more, including seven that went right through the geysers at the south pole,” said Linda Spilker, Cassini project scientist at NASA’s Jet Propulsion Laboratory, Pasadena, California.

By following the trail of scientific breadcrumbs, Cassini eventually found that Enceladus harbors a global ocean of salty water under its icy crust, possibly with hydrothermal vents on its seafloor. The trail of clues that began with a puzzling magnetometer reading led to an understanding that the moon — and perhaps many small, icy moons like it throughout the cosmos — could potentially have the ingredients needed for life.

“Half the excitement of doing science is that you sometimes find yourself going in a totally different direction than you expected, which can lead to amazing discoveries,” said Spilker. “That little anomaly in Cassini’s magnetometer signal was unusual enough that it eventually led us to an ocean world.”

For a timeline of Cassini’s Enceladus discoveries, visit: http://go.nasa.gov/2k0CRP3

Launched in 1997, the Cassini mission is currently in its final year of operations, performing weekly ring-grazing dives just past the outer edge of Saturn’s rings. In April, the spacecraft will begin its Grand Finale, plunging through the gap between the rings and the planet itself, leading up to a final plunge into Saturn on September 15.

Illustration showing the bending of Saturn’s magnetic field near Enceladus that was detected by Cassini’s magnetometer. Credit: NASA/JPL-Caltech > Full image and caption

Cassini has been touring the Saturn system since arriving in 2004 for an up-close study of the planet, its rings and moons, and its vast magnetosphere. Cassini has made numerous dramatic discoveries, besides the activity at Enceladus, including liquid methane seas on another moon, Titan.

The Cassini-Huygens mission is a cooperative project of NASA, ESA (European Space Agency) and the Italian Space Agency. NASA’s Jet Propulsion Laboratory, a division of Caltech in Pasadena, California, manages the mission for NASA’s Science Mission Directorate, Washington. JPL designed, developed and assembled the Cassini orbiter.

More information about Cassini:

Curiosity sharpens contrast of a watery surface and a thin atmosphere on early Mars

The full-sized image of the Yellowknife Bay Formation on Mars looks like you could just walk right out onto it. (But wear a spacesuit if you do.) In this article, spots like Yellowknife are providing insights as well as contradictions about the conditions of the planet in its early eons:

NASA’s Curiosity Rover Sharpens Paradox of Ancient Mars

Bedrock at this site added to a puzzle about ancient Mars by indicating that a lake was present, but that little carbon dioxide was in the air to help keep a lake unfrozen. Full image and caption

Mars scientists are wrestling with a problem. Ample evidence says ancient Mars was sometimes wet, with water flowing and pooling on the planet’s surface. Yet, the ancient sun was about one-third less warm and climate modelers struggle to produce scenarios that get the surface of Mars warm enough for keeping water unfrozen.

A leading theory is to have a thicker carbon-dioxide atmosphere forming a greenhouse-gas blanket, helping to warm the surface of ancient Mars. However, according to a new analysis of data from NASA’s Mars rover Curiosity, Mars had far too little carbon dioxide about 3.5 billion years ago to provide enough greenhouse-effect warming to thaw water ice.

The same Martian bedrock in which Curiosity found sediments from an ancient lake where microbes could have thrived is the source of the evidence adding to the quandary about how such a lake could have existed. Curiosity detected no carbonate minerals in the samples of the bedrock it analyzed. The new analysis concludes that the dearth of carbonates in that bedrock means Mars’ atmosphere when the lake existed — about 3.5 billion years ago — could not have held much carbon dioxide.

“We’ve been particularly struck with the absence of carbonate minerals in sedimentary rock the rover has examined,” said Thomas Bristow of NASA’s Ames Research Center, Moffett Field, California. “It would be really hard to get liquid water even if there were a hundred times more carbon dioxide in the atmosphere than what the mineral evidence in the rock tells us.”

Bristow is the principal investigator for the Chemistry and Mineralogy (CheMin) instrument on Curiosity and lead author of the study being published this week in the Proceedings of the National Academy of Sciences.

Curiosity has made no definitive detection of carbonates in any lakebed rocks sampled since it landed in Gale Crater in 2012. CheMin can identify carbonate if it makes up just a few percent of the rock. The new analysis by Bristow and 13 co-authors calculates the maximum amount of carbon dioxide that could have been present, consistent with that dearth of carbonate.

In water, carbon dioxide combines with positively charged ions such as magnesium and ferrous iron to form carbonate minerals. Other minerals in the same rocks indicate those ions were readily available. The other minerals, such as magnetite and clay minerals, also provide evidence that subsequent conditions never became so acidic that carbonates would have dissolved away, as they can in acidic groundwater.

The dilemma has been building for years: Evidence about factors that affect surface temperatures — mainly the energy received from the young sun and the blanketing provided by the planet’s atmosphere — adds up to a mismatch with widespread evidence for river networks and lakes on ancient Mars. Clues such as isotope ratios in today’s Martian atmosphere indicate the planet once held a much denser atmosphere than it does now. Yet theoretical models of the ancient Martian climate struggle to produce conditions that would allow liquid water on the Martian surface for many millions of years. One successful model proposes a thick carbon-dioxide atmosphere that also contains molecular hydrogen. How such an atmosphere would be generated and sustained, however, is controversial.

The new study pins the puzzle to a particular place and time, with an on-the-ground check for carbonates in exactly the same sediments that hold the record of a lake about a billion years after the planet formed.

For the past two decades, researchers have used spectrometers on Mars orbiters to search for carbonate that could have resulted from an early era of more abundant carbon dioxide. They have found far less than anticipated.

“It’s been a mystery why there hasn’t been much carbonate seen from orbit,” Bristow said. “You could get out of the quandary by saying the carbonates may still be there, but we just can’t see them from orbit because they’re covered by dust, or buried, or we’re not looking in the right place. The Curiosity results bring the paradox to a focus. This is the first time we’ve checked for carbonates on the ground in a rock we know formed from sediments deposited under water.”

The new analysis concludes that no more than a few tens of millibars of carbon dioxide could have been present when the lake existed, or it would have produced enough carbonate for Curiosity’s CheMin to detect it. A millibar is one one-thousandth of sea-level air pressure on Earth. The current atmosphere of Mars is less than 10 millibars and about 95 percent carbon dioxide.

“This analysis fits with many theoretical studies that the surface of Mars, even that long ago, was not warm enough for water to be liquid,” said Robert Haberle, a Mars-climate scientist at NASA Ames and a co-author of the paper. “It’s really a puzzle to me.”

Researchers are evaluating multiple ideas for how to reconcile the dilemma.

“Some think perhaps the lake wasn’t an open body of liquid water. Maybe it was liquid covered with ice,” Haberle said. “You could still get some sediments through to accumulate in the lakebed if the ice weren’t too thick.”

A drawback to that explanation is that the rover team has sought and not found in Gale Crater evidence that would be expected from ice-covered lakes, such as large and deep cracks called ice wedges, or “dropstones,” which become embedded in soft lakebed sediments when they penetrate thinning ice.

If the lakes were not frozen, the puzzle is made more challenging by the new analysis of what the lack of a carbonate detection by Curiosity implies about the ancient Martian atmosphere.

“Curiosity’s traverse through streambeds, deltas, and hundreds of vertical feet of mud deposited in ancient lakes calls out for a vigorous hydrological system supplying the water and sediment to create the rocks we’re finding,” said Curiosity Project Scientist Ashwin Vasavada of NASA’s Jet Propulsion Laboratory, Pasadena, California. “Carbon dioxide, mixed with other gases like hydrogen, has been the leading candidate for the warming influence needed for such a system. This surprising result would seem to take it out of the running.”

When two lines of scientific evidence appear irreconcilable, the scene may be set for an advance in understanding why they are not. The Curiosity mission is continuing to investigate ancient environmental conditions on Mars. It is managed by JPL, a division of Caltech in Pasadena, for NASA’s Science Mission Directorate, Washington. Curiosity and other Mars science missions are a key part of NASA’s Journey to Mars, building on decades of robotic exploration to send humans to the Red Planet in the 2030s. For more about Curiosity, visit: www.nasa.gov/curiosity

Blue jets and red sprites observed from the ISS

Blue and red lightning bolts shooting upwards from high altitude clouds have been observed from the International Space Station and recorded on video: Blue jets studied from Space Station – ESA

Screen capture from video of blue jet of lightning as seen from the ISS.

For years, their existence has been debated: elusive electrical discharges in the upper atmosphere that sport names such as red sprites, blue jets, pixies and elves. Reported by pilots, they are difficult to study as they occur above thunderstorms.

ESA astronaut Andreas Mogensen during his mission on the International Space Station in 2015 was asked to take pictures over thunderstorms with the most sensitive camera on the orbiting outpost to look for these brief features.

Denmark’s National Space Institute has now published the results, confirming many kilometre-wide blue flashes around 18 km altitude, including a pulsating blue jet reaching 40 km. A video recorded by Andreas as he flew over the Bay of Bengal at 28 800 km/h on the Station shows the electrical phenomena clearly – a first of its kind.

The Station’s low orbit makes it an ideal platform from which to observe and study these unusual electrical atmospheric phenomena. In the video below,

ESA astronaut Andreas Mogensen explains the phenomena he filmed over India from the International Space Station’s Cupola observatory in September 2015 during his postflight tour at ESA’s technical heart ESTEC in The Netherlands.

The film shows lightning illuminating clouds and recently discovered phenomena called blue jets and Red Sprites.

As part of his 10-day mission Andreas performed an experiment called Thor after the god of thunder, lightning and storms in Nordic mythology. Initiated by the Technical University of Denmark, Thor had Andreas test a new thundercloud imaging system that looks at the electrification of lighting.

Researchers are particularly interested in newly-discovered lights that occur in the upper atmosphere during thunderstorms called red sprites, blue jets and elves. Sprites last 20 milliseconds at most, and to capture them on camera is a real challenge. They received their name because of their elusive nature. Blue jets are found up to 50 km altitude with Red Sprites occurring between 60-80 km altitude.

Andreas received the coordinates of a few possible thunderstorms together with the times and instructions on which lens, filter and camera settings to use.

Some of the most violent electric discharges are very difficult to capture from the ground because the atmosphere blocks radiation. Apart from covering all the main thunderstorm regions, the International Space Station brings scientists as close as possible to the electric phenomena. Its great vantage point has the lowest orbit available for observation at around 400 km altitude – imaging satellites mostly operate at 800 km.

Read more about Andreas’s iriss mission: http://www.esa.int/iriss

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Images of dunes and gullies on a Mars crater wall

The Mars Reconnaissance Orbiter sends a terrific view of dunes and gullies formed on a crater wall on the Red Planet:

The Contrasting Colors of Crater Dunes and Gullies 

Gullies are relatively common features in the steep slopes of crater walls, possibly formed by dry debris flows, movement of carbon dioxide frost, or perhaps the melting of ground ice.

This example shows a section of crater wall from the rocky crater rim at the far left of the image, down to the dark dusty dunes on the crater floor in the bottom right. (North is to the left.) The rock of the crater walls shows up deep orange, and the sandy deposits on the crater floor and the base of the crater walls appear blue. The sand isn’t really blue; the different colors in this image represent different material compositions.

The gullies in this image have two main sections: a scalloped alcove at the top of the gully (left/center), and defined channel sections further down the crater wall (right/center). Material from the alcove will have traveled down the channel to the crater floor. This normally forms a third section to a typical gully, a debris fan. Fans commonly visible at the base of gullies are not obvious in this example however, as the wind blown sediments (blue) have covered the crater floor after gully formation.

The University of Arizona, Tucson, operates HiRISE, which was built by Ball Aerospace & Technologies Corp., Boulder, Colo. NASA’s Jet Propulsion Laboratory, a division of Caltech in Pasadena, California, manages the Mars Reconnaissance Orbiter Project for NASA’s Science Mission Directorate, Washington.

Hi-Rise raw image. Click for larger version

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Cassini views the little moon Daphnis up close

In early January, the Cassini spacecraft took this marvelous shot of the small moon Daphnis as it travels along in a gap in Saturn’s rings: Cassini: Mission to Saturn: Daphnis Up Close 

The wavemaker moon, Daphnis, is featured in this view, taken as NASA’s Cassini spacecraft made one of its ring-grazing passes over the outer edges of Saturn’s rings on Jan. 16, 2017. This is the closest view of the small moon obtained yet. Daphnis (5 miles or 8 kilometers across) orbits within the 42-kilometer (26-mile) wide Keeler Gap. Cassini’s viewing angle causes the gap to appear narrower than it actually is, due to foreshortening. The little moon’s gravity raises waves in the edges of the gap in both the horizontal and vertical directions. Cassini was able to observe the vertical structures in 2009, around the time of Saturn’s equinox. [Full caption and larger images]
Check out the latest Cassini shots from the Saturnian system in the Mission to Saturn Images gallery and the Raw Images gallery

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