Chasing the aurora from the world’s northernmost rocket range

Part VI
I • II •​ ​III •​ IV •​ ​V •​ VI​ •​ VII

Doug Rowland. Credit: NASA/Joy Ng

On the snow-covered balcony, the science team huddled together in t-shirts and indoor slippers, too rushed to don their coats. Everyone was there except Rowland.

The first rocket was already in the air, but many on the team — glued to their computers until the last moments — had missed it. The flight of the second rocket would be their first chance to see the launch.

“Thirty seconds,” an unidentified voice called from inside.

The hall door opened. With only a few moments left, Rowland made his way into the huddle. The crowd lifted their phones to capture the event, but all eyes were off in the distance, staring toward the launchpad. Suddenly, all faces were illuminated. A collective sigh rose up as an intensely bright flash illuminated the terrain. Ny-Ålesund was surrounded by mountains — for the first time, they could see them.

The second VISIONS-2 rocket launches. Credit: NASA/Joy Ng

The bright orb lifted quickly into the sky, followed a few moments later by a thunderous rumble. The trail of light continued on its arc as heads craned out over the balcony. The light began to dim, then suddenly brightened again. “Second stage!” Pfaff called out, to hollers of approval. Then the rocket passed out of view.

Without a word, the entire crowd rushed for the door, running back to their computers to watch the data stream in.  As they took their places, Rowland hovered among them like a conductor surveying his orchestra.

“First images!” he called out, pointing at a screen at the first station. It was the CCD imager, nitrogen-cooled, that was now flashing images in four square boxes, arranged two-by-two on the screen. At first, they each flickered rapidly, unsynchronized. Then suddenly, a semicircle of bright light appeared in all of them. “We’ve got the limb of the Earth!” he cried — the horizon was in view. The rocket was in space, looking back down at them.

Rowland continued down the line. Next up was a particle counter, measuring the oxygen ions escaping the atmosphere as the rocket flew through them. “We got the counts?” he called. Zaccarine, still glued to her screen, raised a thumbs-up.

Rowland scanned the room. Scientists watched their data roll in, narrating each dip and turn to one another like sports announcers. Radio chatter crackled in the background. At just under four minutes into the flight, all of the instruments were on, and no problems had been reported. Rowland stood, hands on the back of an empty seat, as his eyes welled with tears. A team member reached for a handshake but Rowland went for a hug.

Moen and Pfaff, the two veterans, met him in the middle of the room for congratulations. “Everything seems to be working,” Rowland said. He smiled and looked at Pfaff. “Looks like you might make your conference after all.”

Long-exposure photo of the 39 and 40 rocket launches. Credit: NASA/Allison Stancil-Ervin

Continue to Part VII



Chasing the aurora from the world’s northernmost rocket range

Part V
I • II •​ ​III •​ IV •​ ​V •​ VI​ •​ VII

Rob Pfaff. Credit: NASA/Joy Ng

Pfaff paced in front of the Wall of Science, stroking his chin, weighing the signs that launchable conditions were approaching. He had spent earlier hours on the phone, rapidly rebooking flights to make his science conference on time. But that was earlier, when conditions weren’t good. Now, everyone was at full attention.

In the background, the tinny sound of voices over a video chat trickled in. Moen, the professor from Oslo, was speaking with colleagues 50 miles south in Longyearbyen. One voice belonged to Fred Sigernes, Chief of the Kjell Henriksen Observatory, who was running the all-sky imager, the instrument that detected the cusp on the Wall of Science. The other voice belonged to Kjellmar Oksavik, a professor at the University of Bergen and at UNIS in Svalbard. He was running the EISCAT radar, scanning the sky for atmospheric heating. They kept the line open as they worked, ready to discuss every bit of new data as it appeared, in real time.

One of two EISCAT radar antennas in Longyearbyen. Credit: NASA/Joy Ng

At 11 a.m. — with one hour left in the day’s launch window — the solar wind’s magnetic field started to point south.

Rowland, sensing the opportunity to launch may be drawing close, OK’d the launch team to arm the rocket. “Let’s run the clock down to three minutes,” he said. It was as close to zero as they could get. Below that, the rocket was switched to internal battery power and the engineers completed their final checks.

Fifteen minutes passed and the solar wind’s magnetic field was still pointing south, but always zig-zagging, threatening to head north at any moment. The red blob marking the cusp remained too far north above Ny-Ålesund to launch through. A call came in over a walkie-talkie, and Rowland picked it up.

“We have some concern about surface winds.” It was Range Control. “It is not really stable enough just yet, and they are quite high. If you see something you want to start the count for, we will have to assess the winds at that point to make a decision if we can go or not.”

Rowland paused, working through his options. The cusp was still too far north at the moment, but given the steady stream of southward-pointing solar wind hitting Earth, it was due to move any moment. Once it moved into the rocket’s trajectory, they needed it to heat the atmosphere before they’d be ready to launch. “We’ll let it cook for a few minutes,” Rowland responded, “and then we’ll pick up the count.”

Zaccarine stands over her computer as launch opportunity draws near. Credit: Miles Hatfield

Before Rowland finished his sentence, Pfaff was already gesturing to him. “It’s slowly moving south,” he said. They rushed out to the Wall of Science, and Pfaff pointed to the red blob marking the cusp. “This used to be up here, now it’s right on top of us.”

By 11:50 a.m., with just ten minutes left in the launch window, the atmosphere was starting to heat up. The EISCAT radar’s measurements, once cool blues and greens, were turning orange and yellow. Now, time was of the essence.

“It’s three minutes to get in the air, and another couple to get to apogee — we’re five minutes from measuring anything,” said Rowland. It wasn’t the data now, but five minutes into the future, that they depended on. Rowland turned to Moen, who spoke to his colleagues over the video chat. “Should we go?” Moen asked.

Rowland looked around to the surrounding science team. The stakes were high enough to demand a unanimous decision. If they launched toward a transient, momentary fluke of heating that disappeared before they reached it, three years of work on the mission would be wasted. But waiting too long could lead to a similar fate if they missed their only chance. “Any dissenters?” he asked.

A hushed discussion ensued over the video chat as Rowland, out of earshot, studied the Wall of Science. Pfaff leaned in to the computer to listen closely. “They’re saying go!” Pfaff yelled. Everyone turned to Rowland. That was all the resolution he needed.

Rowland notified Range Control of their decision to launch and rushed back to the Wall of Science. At the bottom left display, the clock, long frozen at three minutes, began to count down.

Continue to Part VI



Chasing the aurora from the world’s northernmost rocket range

Part IV
I • II •​ ​III •​ IV •​ ​V •​ VI​ •​ VII

Jøran Moen. Credit: NASA/Joy Ng

Each day, the science team prepared just the same. At 3 a.m., Rowland opened the giant doors of the Telemetry Readout building, where they were stationed. Over the next five hours, they stepped through instrument preparations, tests, and practice countdowns. It had now reached 8 a.m. on the fourth day of the launch window. Practice was over — it was time to try, once more, for the real thing.

Rowland sat in the front room of the building, hunched over his laptop. Two long tables stretched out to either side of him, stacked with computer monitors of different shapes and sizes. Streams of data danced across their screen, one for each of the 11 instruments on the rocket. These were the rocket’s vital signs, so they watched them meticulously, beginning long before launch. Beside Rowland, Zaccarine, the youngest member of the science team, stared at the temperature readouts from one of the instruments that she’d watched for three days now.

The science team monitors their instruments in the Telemetry Room. Credit: NASA/Joy Ng

Across the room, Pfaff inspected long sheets of paper showing data from several instruments. Pfaff was familiar with the challenges of launching from Ny-Ålesund, and could advise Rowland on what to look for. But he couldn’t stay long. He was scheduled to deliver two lectures at a science conference back in Washington, D.C., and had almost left that morning. At the last minute, he delayed his flight: The weather seemed promising today.

The rest of the team gathered in the adjacent main hall. Jøran Moen and Andres Spicher from the University of Oslo, a professor and postdoc respectively, sat at a small table, sipping coffee from skinny white mugs. Moen was in charge of one of the instruments, but he also knew the cusp region well. He was one of the chief architects of the Grand Challenge Initiative – Cusp, the international sounding rocket campaign to explore the cusp, of which Rowland’s mission was one part.

Across the room, Matt Zettergren, a professor from Embry-Riddle, was fiddling with cables dangling from his laptop. One clicked into place, and a large screen in the middle of the room came alive. Four scientists gazed up at it, their faces illuminated by the blue-white glow.

The science team in front of the Wall of Science. Credit: NASA/Joy Ng

This was the Wall of Science, as they playfully called it. Its geometric arrangement of windows resembled farmland seen from a plane. The separate plots of data were beamed back from satellites in space and ground-based instruments. They blinked, shifted, and refreshed each at their own cadence. But each parcel had its own significance, requiring the right attention and know-how to read it. The Wall of Science contained all the information they had to decide whether, and when, to launch.

“This is our upstream space weather buoy,” said Rowland, pointing to a window in the upper right-hand corner of the screen. It was one of three windows that, together, told the story of atmospheric escape, following a gust of solar wind as it approached Earth, flowed through cusp, and triggered the aurora and fountains of escaping oxygen.

The first window showed a red squiggly line stretching across the plot. The data came from NASA’s Advanced Composition Explorer, or ACE satellite, perched one million miles closer to the Sun than we are. The science team looked to this data to see what the solar wind was blowing their way, some 45 minutes to an hour before it hit Earth.

This red squiggly line measured the solar wind’s magnetic field. Like Earth itself, the solar wind is magnetic, with its own north and south pole. But while north, on Earth, points in one steady direction, the solar wind is far less stable. A compass placed inside it would spin from moment to moment, depending on the changing activity on the Sun.

The scientists were waiting for the solar wind to point south, and to stay that way for a while. When a southward-pointed solar wind collided with Earth’s northward-pointed magnetic field, the two would fuse. It was the first step toward the ideal cusp aurora.

The effects of this collision could be seen on Earth, and were displayed in the next window. In two wavelengths of red light emitted by the aurora, it showed the location of the cusp over Svalbard.

At the moment, the cusp was positioned to the northeast of the island, out of range of the rockets’ trajectory. But the arrival of a southward-pointing gust of solar wind would intensify the aurora, dragging the cusp southward, towards the rocket’s planned trajectory.

Once the cusp started shifting south, launchable conditions were closing in. But to fire the rockets, the science team looked to the final window, placed on the far left of the screen. It told them when the aurora had reached its boiling point, and the oxygen was starting to escape. The data were from the EISCAT radar, short for European Incoherent Scatter Scientific Association. The two EISCAT antennas measured the density and temperature of the atmosphere over Ny-Ålesund, and at the peak of the rocket’s trajectory. When oxygen in the air started to boil, they would see it here. It would be time to start the countdown.

There was one more window squeezed into the bottom left corner, the only one that the team itself controlled. It was a simple digital clock. When it struck zero, rockets would fly.

Continue to Part V



Chasing the aurora from the world’s northernmost rocket range

Part III
I • II •​ ​III •​ IV •​ ​V •​ VI​ •​ VII

Sophie Zaccarine explains atmospheric escape. Credit: NASA/Joy Ng

At the entrance to the mess hall, Ny-Ålesund residents abandon snow-covered shoes for cozy slippers or socks. Inside, the warm air washes over wind-whipped faces, carrying the smell of rich soups, tea, and bread. “The chef is the most important person here,” Rowland quipped.

Residents make the pilgrimage to the mess hall three times a day: first for breakfast, beginning at 7:30 a.m. sharp, then for lunch, which runs from 12:20 to 1, and finally dinner from 4:50 to 5:30. Meals are not served outside of those hours, so the mess hall’s schedule is the town’s heartbeat. It also makes for a reliable meeting ground — a place hungry colleagues gather to discuss the day’s events.

The science team sat together at a table for lunch. The launch window on the second day had just closed — another scrub — but this time it wasn’t the wind. Instead, the aurora had eluded them.

In broad strokes, all types of aurora have a similar origin story. They form when negatively charged electrons crash into the gases in our atmosphere, jarring those gases into high-energy states. As they relax back to normal they give off their excess energy in the form of light: the ruby reds and emerald greens that illuminate the northern and southern skies.

Most of these auroras are formed by the same population of electrons. These electrons come from inside Earth’s magnetic field.

Illustration of the Earth’s magnetosphere, polar cusps and the solar wind. The northern and southern polar cusps appear as two funnels, where the solar wind can collide with Earth’s atmosphere. The collisions create the cusp aurora and hot fountains of outflowing oxygen. Credit: NASA CILab/Josh Masters

But the cusp auroras — the kind that form above Ny-Ålesund for just a few hours a day — are from a different stock of electrons. When they set the sky alight, they are at the end of a 93-million-mile journey, direct from the Sun.

Most particles that flow off the Sun — collectively known as the solar wind — don’t have that fate. By and large, they are deflected around Earth’s magnetic field, sent skimming off into space. But near the north and south poles, there are two funnels where solar particles can slip inside.

These holes in our protective shield are known as the polar cusps. They’re the only places on Earth where the oncoming solar wind directly collides with our atmosphere. The polar cusps are anchored to the Sun-facing side of Earth; as the planet rotates, they remain in perpetual daylight, piping  electrons from the Sun into the polar atmosphere. And between the hours of 10 a.m. and noon, the town of Ny-Ålesund passes right beneath one of them.

The cusp aurora hold secrets that extend far beyond Ny-Ålesund, both in space and time. Some 4.2 billion years ago, Mars had a hearty atmosphere along with liquid water on its surface. In its prime, scientists estimate, it might have been suitable for life. But through the millennia, the solar wind stripped Mars’s atmosphere to produce the exposed, barren landscape we see today. Partly, this is due to Mars’s weak magnetic field, which is unable to protect the planet as well as Earth’s can. Yet the story is more complicated than that, for Venus’s magnetic field is also weaker than Earth’s, yet it boasts an atmosphere 90 times thicker.

A planet’s fate lies in a complicated balancing act between countless physical processes, some that drain its atmosphere away and some that grow it. In the cusp aurora, some of these processes can be spied up close.

The cusp aurora. Credit: Bin Li

But Rowland is also looking to the future. Today, with just over 4,000 confirmed exoplanets, or planets orbiting stars elsewhere in the universe, the race is on to determine which of them are potentially habitable. But the dynamics of their atmospheres — which make or break their suitability for life — remain poorly understood. At present, we can do no more than make intelligent guesses, based on scientific models, about what their atmospheres might be like. To check the accuracy of these models, we test them with data collected on Earth. Data just like what Rowland’s team were here to get.

But there were no guarantees that the cusp auroras would cross their path. When the Sun’s activity is low, the cusp passes just north of Ny-Ålesund, outside of their approved launch trajectory. But a healthy gust of solar wind, they knew, could push it south, right into their path. So they waited, readying their rockets to ambush the aurora at the perfect moment.

Continue to Part IV



Chasing the aurora from the world’s northernmost rocket range

Part II
I • II •​ ​III •​ IV •​ ​V •​ VI​ •​ VII

Glenn Maxfield, launcher systems manager, walks to the blockhouse. Credit: NASA/Joy Ng

At 3:45 am, the van rumbled over a snow-covered road away from the team’s dormitories. The launchpad was a ten-minute ride outside the town limits. Ny-Ålesund’s boundaries are marked with triangle-shaped signs, outlined in red, encasing the silhouette of a polar bear. “STOP!” they read, “Do not walk beyond this sign without your firearm.”

Ny-Ålesund’s boundaries are marked with polar bear warning signs. Credit: NASA/Joy Ng

So far, residents had delivered nothing more than warning shots, but that summer’s 11 polar bear sightings kept them on their guard. Lately, the biggest nuisance had been a large male, nicknamed Whitey, who destroyed several of the vacation cabins used during warmer months. Half-joking “Wanted” posters hanging inside the mess hall show a picture of him, snout protruding through a cabin window. He is on the inside, looking out.

As the van approached the launchpad, tufts of snow skimmed across the ground like tiny clouds on a miniature landscape. The chassis hummed from the wind’s vibration — it was gusting hard today.

Today was the first of 15 opportunities to launch. Day 1 launches do happen occasionally. But for some missions, even two weeks won’t beget the combination of clear weather, pristine aurora, and no engineering issues. It’s not unheard of for entire teams to pack up and try again next year.

Across the snow, two yellow scaffolding towers aimed themselves skyward at a forty-five-degree angle. These were the launchers, and on the underside of each, encased in a Styrofoam shell, was a ready-to-launch rocket. Named by shortening their mission number, the nearest rocket was “39,” and behind it, “40.”  Together, they comprised the VISIONS-2 mission.

One of two launchers, carrying a rocket covered by Styrofoam to protect it from the weather. Credit: NASA/Joy Ng

These were sounding rockets — so-called for the nautical term “to sound,” meaning “to measure.” They vary in size, but can stand up to 65 feet tall and are usually just slim enough for a bear-hug. Sounding rockets fly anywhere from 30 to 800 miles high, carrying scientific instruments into space before falling back to Earth. The two on the launchpad carried 11 instruments between them. One rocket would spin through its flight, gathering data from all viewing angles, while the other would steady itself after launch for those experiments that required a stable view. They would launch two minutes apart along a southward trajectory, peaking around 300 miles high and landing some 15 minutes later in the Greenland Sea.

The rockets and their launchers are controlled from the blockhouse, a modest building 100 yards from the launchpad. Inside, a burly man with a bushy beard stood in the middle of a tiny room, surrounded by eight engineers. Glenn Maxfield, the launcher systems manager, was one of the leaders of the team. He spent much of his time outside, with the rocket. But right now, he and the rest of the team were staring at a temperature gauge. Something was wrong.

The temperature gauge monitored a special camera aboard one of the rockets known as a charge-coupled device, or CCD. The CCD camera would capture imagery of the aurora as the rocket flew through it. But to work properly, it had to be cold — below -31 degrees Fahrenheit. Too warm and it would ruin their view of the aurora, producing “dark noise” that resembles an overexposed photograph.

To keep it cold the team was using a liquid nitrogen cooling system. But nitrogen was now pooling at a U-turn in the plumbing inside the rocket. If it wasn’t fixed, the instruments could cool so quickly they could fracture.

Maxfield was on the phone with Range Control, the team that coordinated launch operations.  Range Control, noting increasing winds, wanted to lower the rockets from their ready-to-launch positions.

“Right now, I don’t know how much nitrogen is in there, and if we go down, there’s the potential that it runs into the instruments,” Maxfield said. But the solution was already in the works. Maxfield had opened a valve to allow excess nitrogen to evaporate out from the rocket; he could hear it hiss as it steamed away. Now, they just had to wait. He hung up the phone and headed back out to the rocket.

A few moments later Maxfield returned, looking satisfied. The hiss had stopped. The liquid was gone, and the CCD camera had reached the target temperature. “I think we’re good,” he said.

Doug Rowland. Credit: NASA/Joy Ng

Sounding rockets “go where you point them,” Rowland said. “Unless it’s windy. Then they go somewhere else.”

The success of a sounding rocket mission depends on fixing just these kinds of problems as they arise. But it’s at least as dependent on the weather, which is much harder to control. Ground winds could endanger a rocket still on the launchpad, but winds higher up were at least as threatening. For all their complicated mechanics, sounding rockets have no rudder, no real-time ability to steer once they’re in flight. Sounding rockets “go where you point them,” Rowland, the mission leader, said. “Unless it’s windy. Then they go somewhere else.”

So the team doesn’t take chances: The launch systems could accommodate winds up to 20 miles per hour, but no more. Gusty conditions could send the team home for the day. A prolonged storm could squander their entire two-week window.

Monitoring those winds was the job of Anders Moen and Tommy Jensen, both employees of the Andøya Space Center, the Norwegian agency responsible for operating the range. Inside the blockhouse, they were tracking a weather balloon. Their screen displayed a simplified map of Svalbard, with Ny-Ålesund at the center. A thin line squiggled across Ny-Ålesund to a point somewhere over the Arctic Ocean, marking the balloon’s current location. It was almost out of range — about time to launch another.

Moen and Jensen got up and continued into the neighboring open hangar. Next to its rolling door was a collection of giant metal gas tanks. Jensen reached for one, turned the dial, and a hollow hissing sound began. He held up a white balloon from his fist, which hung first like an empty bag then righted itself, filling rapidly until reaching a 5-foot diameter. Moen tied it to a GPS device — a small white box about the size of a paperback novel. Jensen pushed a button on the wall and the large rolling door opened.

Outside the hangar, the wind was loud, and snow tussled in front of them like tumbleweed. Jensen raised his arm, waiting for a signal on his walkie-talkie, as Moen carried the white box. A moment’s pause, a walkie-talkie confirmation, and he let it free. With a loud tearing sound, it took off like a dragster as the white box jerked from Moen’s hand, whipping frantically after the balloon. Shooting off at a diagonal, the balloon quickly disappeared into the darkness.

Anders Moen and Tommy Jensen release a weather balloon. Credit: NASA/Joy Ng

During launches, Moen and Jensen carried out this ritual several times a day. After release, the GPS device would send real-time data showing the balloon’s altitude, speed, and direction that allowed them to monitor high-altitude winds. In a few moments, a new line would trace across Moen and Jensen’s monitor. They turned and walked back into the hangar as the rolling door closed behind them.

Soon after, the signal from the newly launched GPS balloon was coming in, and the news wasn’t good. It was showing gusts at 37 miles per hour, well above their cutoff. Range Control radioed in and recommended “scrubbing,” or ending the launch attempt for the day. Shortly afterward, Rowland made it official.

Day 1 was over, rockets still on the ground.

Continue to Part III



Chasing the aurora from the world’s northernmost rocket range

In the tiny Arctic town of Ny-Ålesund, where polar bears outnumber people, winter means three months without sunlight. The unending darkness is ideal for those who seek a strange breed of northern lights, normally obscured by daylight. When these unusual auroras shine, Earth’s atmosphere leaks into space.

NASA scientists traveled to Ny-Ålesund to launch rockets through these auroras and witness oxygen particles right in the middle of their escape. Piercing these fleeting auroras, some 300 miles high, would require strategy, patience — and a fair bit of luck. This is their story.

Listen to this story

Part I
I • II •​ ​III •​ IV •​ ​V •​ VI​ •​ VII

The only plane to Ny-Ålesund departs twice a week, on Mondays and Thursdays. Credit: NASA/Joy Ng

When the bus finally came to a stop, they found themselves inside a glass-walled garage. A man was standing inside.

“Welcome to Ny-Ålesund!” the man cheered. His messily-parted, shoulder-length brown hair would fit in on tour with a heavy metal band. But this was Doug Rowland, NASA rocket scientist, and the team’s leader. He was the one who had called them to meet in this cold, dark, and strangely beautiful place.

The newcomers stepped off the bus and into the garage’s light. Among the first was Sophie Zaccarine, who waved hello to Rowland with both arms overhead.  A 21-year-old engineering physics major, Zaccarine would monitor one of the scientific instruments during the flight. Over the past three years, she had worked through summer internships and short visits to NASA to design and build a small electronics enclosure that, very soon, would become her first bit of hardware in space. Robert Pfaff strode in later, nodding at staff as he passed them. Pfaff was a co-investigator, in charge of one of the experiments, and a veteran rocket man. He led the very first NASA launch from this remote arctic town in 1997, and has launched more rockets here than anyone else at the agency.

As Rowland greeted each of the 11 new arrivals, he appeared visibly relieved — his science team was finally here. Rowland had been on the island for a few weeks already, helping to reassemble the two rockets after they had traveled across the Atlantic Ocean in pieces, by cargo ship. Today, after three years of development, they now stood fully-assembled and ready at the launchpad a few miles away. But soon they would be much farther, some 300 miles high, flying through an aurora. If all went as planned.

The science team had landed in Ny-Ålesund, the northernmost civilian settlement in the world. A tiny research town on the Norwegian Archipelago of Svalbard, it is a place where trees do not grow. The only fresh food arrives by cargo ship after a voyage across arctic waters. During winter months, Ny-Ålesund’s resident population drops to 30 for the dark season, which is when the team had arrived. It was December. For the next three months, the Sun wouldn’t rise.

Daytime darkness was important, for only against a dark backdrop could the special aurora borealis they sought be seen with the naked eye. But the main reason for coming to this place was not the dark sky, per se. It was what transpired far above it.

Aurora over Ny-Ålesund, bisected by a LIDAR beam. Credit: NASA/Joy Ng

Between the daytime hours of 10 a.m. and noon, a magnetic portal to space passes over Ny-Ålesund. For those two hours, the barrier between sky and space is at its thinnest. Energetic particles normally deterred by Earth’s magnetic field rush into Ny-Ålesund’s air. They strike atmospheric gases, setting the sky alight with auroras that shine during the day. But the strangest thing about these auroras is not visible at all. Inside them, gases are beginning to cook, and some reach their boiling point. Through these auroras, massive amounts of oxygen are boiled away to space.

The process is known as atmospheric escape. It has been happening on Earth for billions of years, and will continue for a billion more — a timescale too long to impact humans. Yet the physical reactions set forth inside these auroras are cogs in the much larger machine of atmospheric change. Over time, they have transformed Earth from a molten ball of magma into the rich, balanced catalyst for life that it is today. To understand atmospheric escape is, in part, to understand how we got here.

So these NASA-funded researchers traveled to Ny-Ålesund to study these auroras and the oxygen they set free. They wanted to understand the precise mechanism of heating, and better quantify exactly how much oxygen is lost this way. In pursuit of these questions, they came armed with the heavy artillery of their trade. They would shoot scientific rockets into the aurora, measuring the oxygen right as it started to escape.

It would take a large team, some sixty-one members in all, each with their own set of skills and responsibilities. Some would monitor the rockets and the precious scientific instruments they carried. Others studied the sky to forecast when to launch. Yet others would coordinate these teams, ensuring each step was taken at the right time and in the proper order. But together, with good timing and a healthy dose of luck, they would attempt to place scientific instruments inside an active aurora. They would watch, up close, how bits of Earth’s atmosphere escape to space.

Continue to Part II

Where Did that Electron Come From?

Tracking Charged Particles into Earth’s Atmosphere with ELFIN

By Mara Johnson-Groh
NASA’s Goddard Space Flight Center

On September 2, 2019 — after a year of quiet conditions in space since its September 2018 launch — a NASA CubeSat the size of a large toaster flew straight through a solar storm, when a burst of material ejected by the Sun dramatically increased the number of highly charged particles coursing through Earth’s magnetic environment.  These observations from the CubeSat — called ELFIN, short for Electron Losses and Fields Investigation — allowed the scientists to see events that are usually too weak to see under normal conditions.

ELFIN’s job, as it circles through Earth’s polar regions, is to measure super-speedy charged particles falling into Earth’s atmosphere, and for the first time, uncover what pushed them there. The highly energetic electrons and ions measured by ELFIN originate in the Van Allen radiation belts, the concentric rings of charged particles trapped around Earth by the planet’s magnetic field. These charged particles can spark aurora, and if strong enough, disrupt telecommunications, so understanding what sends them hurtling towards Earth is important to protecting our assets in space and on the ground.

Here’s what that ELFIN data looked like in the solar storm.

ELFIN observations showed a spike in precipitating charged particles, with warm colors indicating higher numbers, as the satellite flew through a region where the particles were falling down into the atmosphere. Credit: UCLA ELFIN/NASA

The graphs show data over a period of just a few minutes on September 2 with each color (right axis) showing how many particles are present at a given energy (left axis). Red represents higher numbers — and the spike in the middle shows that the particle count was in the millions across a wide range of energies.  Because ELFIN can also determine the direction in which the particles are traveling relative to the Earth’s magnetic field — a measurement known as pitch angle — they can figure out which of these particles are circling around Earth, trapped by the magnetic fields, versus those that are raining down out of the belts toward our planet. ELFIN is the first satellite to quickly survey the whole latitudinal range of the radiation belts with this capability — taking measurements of pitch angle while simultaneously measuring the particles’ energies at high resolution.

In this case, the particles were falling into Earth’s atmosphere as it flew over Norway and the North Sea. Having seen a precipitation event, the scientists looked to see if they could identify what caused it. Particles typically get dislodged by electromagnetic waves pushing them out of orbit. Different waves dislodge particles with different energies or different travel directions. By looking at the distribution of particles that fell into the atmosphere, the scientists hoped to find out which type of wave was responsible. In particular, ELFIN scientists are looking to see if a type of wave known as an electromagnetic ion cyclotron wave, or EMIC wave, can scatter these particles into Earth’s atmosphere. This type of wave typically knocks down only high-energy particles — those with energies above 900,000 electronvolts.

In the ELFIN observations of all pitch angles, there is a distinct spike in the number of particles seen above 900,000 electronvolts (lower panel), which scientists suspect is caused by EMIC waves. Credit: UCLA ELFIN/NASA

The measurements, shown in the bottom panel of the graph above, show a spike of precipitating particles at these high energies, suggesting EMIC waves might be involved. But since it did not also measure EMIC waves, which often occur farther out from where the particles precipitate, the case is not yet closed. The mission expects to answer this question as it continues to collect data over the next one and a half years.

Other NASA missions — like the Magnetospheric Multiscale mission and the Time History of Events and Macroscale Interactions during Substorms mission, which orbit farther out — may be able to collaborate with ELFIN by directly measuring the EMIC waves near the equator that launch the particles, which follow along magnetic field lines all the way down to ELFIN. These types of conjunction measurements from different instruments and vantage points will allow scientists to learn more about EMIC waves scattering phenomena than any single-point observation could.

ELFIN was developed at the University of California, Los Angeles, where over 200 students have contributed to the mission. The mission is funded by NASA and the National Science Foundation.

Machine Learning and the Ionosphere

By Susannah Darling
NASA Headquarters

Imagine, if you will, that you are driving to your favorite restaurant. The traffic is bad, so you use your GPS to find the best route. To get your current location, your phone or GPS listens to a satellite in the Earth’s upper atmosphere. This satellite sends the GPS system information that allows it to determine where you are and the quickest way to get to your destination.

But sometimes, the signal gets interrupted, the GPS won’t load, or it points you in the wrong direction. Why does this happen?

Ryan McGranaghan, space scientist at ASTRA, LLC and NASA affiliate, tried to tackle this problem by figuring out when a GPS is right and when it’s likely to be wrong. To achieve this, McGranaghan turned to observations from past disturbances in GPS signals. He explored how to use machine learning to try and figure out what made it go haywire in each case.

The main thing he was trying to predict was a phenomenon called ionospheric scintillation.  When the electrically-charged part of our atmosphere, known as the ionosphere, becomes too disturbed, it garbles GPS signals that pass through it.

But predicting when a scintillation event is going to happen is no easy task. The atmosphere is a complicated, constantly-changing mix of physics and chemistry, and we still don’t have the ability to consider all factors for predicting when a scintillation event will occur.

To guess the future, look to the past

To start, McGranaghan looked at past data, where we already knew the outcome, and tried to use his algorithm to “guess,” based on a huge number of input variables, whether a given event would cause GPS disruption or not. It’s a bit like solving math problems and then checking your answers at the back of the book.

The graph below shows data on scintillation in the ionosphere. The vertical axis shows a calculation of how disturbed the ionosphere is over time, using data from multiple sources. The higher up on the axis, the more disturbed the ionosphere was at the time. (Click on the graph to see a larger version.)

The ionosphere is never perfectly undisturbed — the dots are always above zero — so the black dashed line on the graph is determined by scientists to mark when communication begins getting disrupted. As you can see, towards the middle of the graph particles in the ionosphere wiggled past the threshold, enough to disrupt satellite signals.

That is where machine learning comes in. McGranaghan trained a support vector machine, or SVM, to try and guess the recipe for a scintillation event.

A Support Vector Machine isn’t a real machine, made of metal and gears. Rather, it’s an algorithm, a mathematical procedure that is used to separate complicated data into two groups. In this case, the support vector machine tried to guess, while only looking at the ingredients and not the outcome, which were “scintillation events” — dots that landed above the dashed line — and which “non-scintillation events,” landing below.

To do this, you have to first give the SVM some training data for it to practice on, where you show it both the ingredients and the outcomes. From this training data, it tries to “learn” (hence “machine learning”) which ingredients tend to produce which kind of outcomes, and then come up with a general rule.

After a lot of the training data is fed into the algorithm and it has had plenty of time to practice, then you give it new data. Now you’re showing just the ingredients, keeping the outcome hidden, and it tries to guess. Based on its experience with the training data, how well does it guess?

Understanding the Results

In the case of ionospheric scintillation events, there are a few different kinds of guesses.

There are the two ways it can be right: guessing it was a scintillation event, and it really was — we’ll call that a hit — or guessing that it wasn’t a scintillation event, and it wasn’t — we’ll call that a correct rejection.  In the graph below, these are color-coded as follows:

Correct responses
Hit – Green
Correct Rejection – Blue

There are two ways to be wrong as well: guessing that there wasn’t a scintillation event, and there was — a miss — and guessing that there was a scintillation event and there wasn’t — a false alarm.

Incorrect responses
Miss – Red
False Alarm – Yellow

After feeding the data to the algorithm, the SVM made its guesses. We’ll now color-code the same data we saw above, but according to this new color scheme:

As you can see, it looks very similar to the previous graph, now in technicolor. Those colors are the result of the SVM identifying scintillation, and scientists marking how “correct” the SVM was.

The dark blue dots reveal where the SVM correctly identified that it was not a scintillation event. If the SVM had incorrectly identified that there was no scintillation event — a miss — the color would be red.

The green dots are cases where the SVM correctly identified that scintillation is happening. Notice that it correctly identified all the dots that were above the dashed line as scintillation events. But also notice the yellow dots. Those mean the SVM incorrectly identified those data points as scintillation — a little overzealous in identifying an event as scintillation. These false alarms mean the SVM is predicting scintillation when it is not occurring, at least not to a degree that would interrupt signals.

The Future of Scintillation Predictions

This is just the beginning of a potentially powerful tool for predicting ionospheric scintillation. In the future, the SVM algorithm could be taught to be more careful about what it labels as scintillation; or, another machine learning algorithm could be applied to get more accurate results.

Regardless, it would be up to the scientist reading the predictions to make the final decisions: both when the scintillation events could occur, and the best way to manage the loss of communication with the satellite.

Friday’s Solar Prominence

By Miles Hatfield
NASA’s Goddard Space Flight Center

On Friday, June 28, NASA’s Solar Dynamics Observatory observed a solar prominence erupting off the limb, or edge, of the Sun.

A solar prominence erupted from the Sun on June 28, 2019. This view comes from SDO’s 304 Angstrom telescope, which shows light emitted from Helium at about 90,000 degrees Fahrenheit. Credit: NASA/SDO/Genna Duberstein

Solar prominences are loops of comparatively cold, dense solar material that become suspended in the Sun’s super-hot outer atmosphere. Because they are colder and denser than their surroundings, they are readily observed by SDO’s 304 Angstrom telescope, shown here. This telescope captures light emitted by Helium atoms at about 90,000 degrees Fahrenheit. The temperature in the surrounding corona, the Sun’s outer atmosphere, can reach a few million degrees Fahrenheit.

Prominences, like most solar eruptions, form over active regions: places where the Sun’s magnetic field is especially intense and complex. Active regions can last for months, making several trips around the Sun (each complete solar rotation is known as a Carrington rotation, and takes about ~27 days). They are difficult to track unless the Sun is close to solar minimum and solar activity is low, as it is now. This active region is currently on its fifth Carrington rotation.

And it has been busy. Just before it began its third rotation in early May, this active region erupted with two back-to-back coronal mass ejections, or CMEs, that were captured by the NASA/ESA Solar and Heliospheric Observatory, or SOHO spacecraft. CMEs are explosions of hot solar material that shoot out from the Sun into space. They are best observed in coronagraph images, like the one shown below, which block out the light from the Sun’s bright surface to observe the dimmer surrounding corona.

A pair of CMEs erupting from Active Region 2740/2741 captured by the SOHO spacecraft. Credit: NASA/ESA/SOHO

To Study the Solar Wind, Cite your Sources

By Miles Hatfield and Lina Tran
NASA’s Goddard Space Flight Center

The solar wind — the hot gas streaming from the Sun — shapes the very space around us.  It douses the solar system in a soup of energetic particles and magnetic fields. It sparks aurora on Earth and Jupiter. It has changed the very habitability of planets — four billion years ago, it blew away Mars’s atmosphere.

Credit: NASA

But there’s still much we don’t understand about the solar wind. As NASA plans to send more spacecraft and astronauts to space, understanding the solar wind is key to protecting them on their journey.

One of the biggest open questions about the solar wind is where, exactly, it comes from. By the time we first detect it with spacecraft close to Earth, the solar wind has already traveled 92 million miles along a winding and convoluted path. Mapping its full journey — from Sun to spacecraft — takes careful measurements and sophisticated computer models.

Here’s how Samantha Wallace, a Ph.D. candidate at the University of New Mexico, does it.

Start with a Magnetogram

The first step is to create a magnetic map of the Sun, since the solar wind travels along the Sun’s magnetic field lines as they spiral outwards from our star.

She starts at the solar surface, known as the photosphere, where the magnetic fields can be imaged with special cameras. But Wallace doesn’t want to image the entire photosphere: She only wants the part that faces the Earth. That’s the only part that blows solar wind towards our planet. (And towards NASA’s Advanced Composition Explorer, or ACE spacecraft, which detects the solar wind.)

But capturing a picture of the Sun’s Earth-facing side isn’t so simple, because the Sun won’t hold still. It rotates by about 13 degrees every day, completing one full revolution — known as a Carrington rotation — about every 27 days.

Scientists like Wallace overcome this challenge by taking snapshots of the Earth-facing side of the Sun as it rotates, day by day. Each snapshot reveals a slightly different portion of the Sun. A new part comes into view while an old part rotates past the horizon. Once the Sun completes a full Carrington rotation, they stitch together the images into a single rectangular plot. The result is a 2-dimensional map that contains information about the entire surface of the Sun at the moment it was facing Earth. It looks something like this:

Credits: NSF/National Optical Astronomy Observatory

This is a magnetic map of the Sun’s photosphere. The top and bottom of the graph are the north and south poles of the Sun, respectively. Along the left and right, the graph depicts the Sun’s Earth-facing surface as it rotated a full 360. Different shades of gray show the strength and direction of the magnetic field. Darker colors are magnetic fields that point in towards the Sun, lighter point away, and medium is a neutral magnetic field.

This map is a start, but it doesn’t tell us where the solar wind truly originates. After it leaves the surface, the hot gas imaged in this map weaves through tangled magnetic fields until it reaches the corona. There, at the Sun’s outer atmosphere, it can escape and become the solar wind.

So, next, Wallace needs to model that coronal magnetic field.

Model the Corona

We don’t have the capability to directly measure the magnetic fields in the corona yet. Instead, scientists use models to predict how the magnetic field at the solar surface transforms as it expands outwards.

Using a model, Wallace estimates the coronal magnetic field. She starts with the observed photospheric field. Then she extrapolates outwards, by a distance about two and a half times the diameter of the Sun, to estimate the coronal magnetic field. Here’s what it looks like:

Credits: NASA/NOAA

The corona’s magnetic field looks much simpler and smoother that the photosphere. On the upper half, the uniform dark gray shows magnetic fields pointing in toward the Sun. On the bottom half, light gray shows magnetic fields pointing away. At the photosphere, depicted in the first graph, the Sun’s magnetic field is complex and rippled. But by the time we reach the corona, that magnetic field has smoothed out as it empties into the solar wind. North and south meet in the middle at the yellow wiggly line. This line marks the heliospheric current sheet, where the Sun’s magnetic field abruptly changes direction.

Connect It to the Spacecraft

Now, when Wallace looks at ACE’s solar wind measurements, she finally has what she needs to cite their sources on the Sun.

Once the solar wind exits the corona, it travels more or less in a straight line. Wallace uses a model that follows individual parcels of solar wind along those straight paths until they reach ACE. Once she connects all the dots, it looks something like this:


Red crosshairs mark which parts of the Sun were directly in front of ACE as it collected measurements. The red vertical lines also note the date when ACE measured a specific parcel of the solar wind.

The yellow lines connect the solar wind that ACE measured at that time to their origins on the surface. As you can see, they come from all over the Sun! Once those parcels of solar wind navigate through the corona, they have already been re-directed quite a bit.

Solve Solar Mysteries

With the 2018 launch of NASA’s Parker Solar Probe, scientists have entered a new era in the study of the solar wind. As Parker passes closer to the Sun than any spacecraft before it, it is observing the solar wind in its freshest state yet. These observations will be key to prying open new questions about the solar wind and the complicated processes on the Sun that produce it.

Credit: NASA SVS/SDO/Tom Bridgman

To prepare for whatever they’ll find in Parker’s data, Wallace and her coauthors used the techniques described here. But the applied it not to ACE, but rather to the second closest spacecraft to the Sun. The German-American Helios mission, launched in 1974, flew as close as 27 million miles from the solar surface. Using archival data, Wallace and her coauthors mapped Helios’s 45-years-old solar wind observations back to the Sun. It was the first time this had ever been done for Helios. The results have already shed light on the nature of the slow solar wind. . . And they also whet scientists’ appetite for the insights that lay ahead as Parker beams its data back to Earth.