Secrets of the Sun

With new tools, scientists are striving to better grasp our star and its potentially widely destructive solar storms. Airing April 25, 2012 at 9 pm on PBS Aired April 25, 2012 on PBS

Program Description



Secrets of the Sun

PBS Airdate: April 25, 2012

NARRATOR: It's an alien landscape, where magnetic tornadoes twist upward, tens of thousands of miles; mysterious dark spots, large enough to engulf the earth, ebb and flow; and violent eruptions shoot tons of charged particles into space, at speeds of over 2,000,000 miles per hour. This is not some strange world on the other side of the galaxy. This is our sun. And now, new technologies are allowing us to see it like never before.

Satellites are giving investigators new insights into centuries old mysteries.

HOLLY GILBERT (NASA Goddard Space Flight Center): That is really a quantum leap in solar physics, a continuous eye on the sun.

NARRATOR: How does our sun work? Where does its power come from? And how can its inner workings impact us, some 93 million miles away? Finding answers has a new urgency. Our sun has a dark side, its violent storms capable of taking down the electrical grids that power our daily lives.

BILL MURTAGH (National Oceanic and Atmospheric Administration Space Weather Center): Repair could take weeks, months and even, worse case scenario, up to 10 years for a full recovery.

JIM GREEN (NASA Planetary Science): If you can imagine a world without electricity, you're really going back in time.

NARRATOR: Now, join scientists on a quest to understand The Secrets of the Sun. Dive deep into its core and ride out its spectacular storms, right now, on this NOVA/National Geographic special.

Dawn; February 15, 2011; Boulder, Colorado: The team at the National Space Weather Prediction Center begins its day, as it usually does, carefully watching the surface of the sun.

Although 93 million miles away, forces here can impact Earth in surprising and destructive ways. Today, after years of relative calm, a satellite detects something, a dramatic explosion on the sun's surface. A violent solar storm that would dwarf Earth is erupting, releasing a massive shockwave, hurtling towards us at over a million miles an hour. Right now, no one is sure what to expect.

BILL MURTAGH: We have to determine when that thing is going to impact Earth's magnetic field. It's going to be sometime tomorrow, perhaps later in the morning, later at night. That's exactly what we're trying to determine. In fact, I have to join the discussions right now, so I'll get back with you.

NARRATOR: The team models the approaching storm. Their simulation shows it racing out from the sun, on the left, towards the small dot on the right, Earth.

The Solar storm carries a one-two punch. First is a solar flare, releasing an outburst of x-rays that can reach Earth within minutes. The second, more ominous threat arrives a few days later, a phenomenon called a coronal mass ejection, or C.M.E. It's a wave of billions of tonnes of electrically charged particles, seen here in this repeating image, as it ripples away from the eye of the storm. Together, they could hit like a cosmic tsunami, delivering a surge of radiation and an electrical spike of trillions of watts, potentially crashing the power grid.

Sound far-fetched? In March, 1989, in Quebec, Canada, that's exactly what happens. One by one, power stations crash, disabled by the overwhelming power surge caused by a C.M.E. wave. In less than two minutes 6,000,000 people are left without power.

Recently, NASA's Jim Green finds evidence that an even bigger solar storm hit Earth in 1859.

JIM GREEN: What we found was the granddaddy of geomagnetic storms, and that was just 150 years ago.

NARRATOR: The reports tell of auroras, brilliant displays in the sky. They are so bright that miners in Colorado wake up and go to work, thinking it is dawn. Other reports tell of a more harmful impact on the lone electrical system of the day, the telegraph.

JIM GREEN: One, for instance, because of the induced current on their system, overheated the battery and started a fire, nearly burned down the telegraph office. Another operator was burned so badly he ended up in the hospital.

NARRATOR: Green uncovers numerous reports of auroras seen, not only across the United States, but around the world. The evidence is clear. Earth was struck by a superstorm in 1859, the result of two massive C.M.E. waves.

JIM GREEN: Those two storms were not only enormous, but they happened one right after the other. No one alive has seen anything like it.

BILL MURTAGH: If we had a geomagnetic storm of that intensity today, the National Academy suggested that the impact on critical infrastructure could be catastrophic. And the big, big concern is the electric power grid.

NARRATOR: The massive electrical surge from a C.M.E. wave could overload power lines and melt transformers, blacking out entire cities.

BILL MURTAGH: Repair could take weeks, months and even, worse case scenario, the National Academy suggested up to 10 years for a full recovery.

JIM GREEN: If that occurred, if you can imagine a world without electricity, we're really going back in time.

NARRATOR: It's not just the power grid that's at risk.

J. TODD HOEKSEMA (Stanford University): More and more, we rely on technology that could be affected by the sun: global positioning satellites, long distance communications, airplane tracking, astronauts in space. So, there's an urgency in understanding what it is that the sun is doing, what's it going to do next? And how can we prepare for that and respond to it?

INTERVIEWER: Worried or not worried?

BILL MURTAGH: Well, I would be just a little bit worried, yeah, concerned right now. We'll be watching it, monitoring it, very closely here in the coming days.

NARRATOR: We've gazed at the sun since antiquity. We've worshipped it and built entire cultures around its power. We marvel when it's eclipsed during the day and when its power lights up the night sky with dancing curtains of light, the aurora. Its power and size are awesome.

It is so huge, a million Earths could fit inside it. Temperatures at its core soar to 27-million degrees Fahrenheit. It's been shining for over four-billion years and will do so for at least four-billion more.

Yet, for something that has such an overwhelming influence on our lives, the sun is mysterious. How does the energy generated in its core reach us as sunlight? What processes are at work inside the sun? And how do these powerful inner workings generate explosive solar storms?

These are some of the mysteries scientists must understand to protect us from the sun's darker side.

JIM GREEN: The sun can really surprise us.

SARAH GIBSON (National Center for Atmospheric Research, High Altitude Observatory): The sun is elusive.

SCOTT MCINTOSH (National Center for Atmospheric Research, High Altitude Observatory): Crazy.

TODD HOEKSEMA: Complicated.


KAREL SCHRIJVER (Lockheed Martin): Incredibly dynamic.


BILL MURTAGH: With explosive potential.

NARRATOR: The key to that explosive behavior lies deep beneath the sun's blinding surface. Until recently, seeing inside the sun was impossible, understanding its internal processes a pipe dream, but an accidental discovery changes everything.

DEAN PESNELL (NASA's Goddard Space Flight Center): Until the 1960s, much of solar physics relied on things that were like solar dermatology. There was, it was things that were right at the surface or just skin-deep.

NARRATOR: But as physicists study the sun in more detail, they make a surprising discovery. The surface seems to be vibrating like ripples on a pond. Initially, they think the vibrations are the result of defective instruments.

DEAN PESNELL: They couldn't get rid of them. They built better instruments, the ripples were still there. They looked at it for 10 years. And at the conferences they all talked about it, and they harrumphed, but what it turned out to be was just sound waves.

NARRATOR: It is an astonishing revelation. No one expects that the sun can generate sound waves. It leads scientists to see the sun in a completely new way.

Our sun vibrates like a giant pipe organ, but instead of air producing the notes, churning gases deep inside send sound waves rippling through its interior.

DEAN PESNELL: Because a sound wave changes as it moves through different material, we can look at the different frequencies and determine what's happening inside the sun.

NARRATOR: Geologists are familiar with this. By studying sound waves passing through the earth's crust, they can see the layers below our feet, a technique called "seismology." Similarly, sound waves moving through the sun's interior reveal how it's made up.

DEAN PESNELL: I can use this organ to illustrate how sound waves work inside the sun. For example, if I hit this low note, it comes from one of these big pipes, big deep sound. And on the sun, that corresponds to a wave that goes very deep into the sun and brings back the information from deep down in the sun. If I turn to a high note, it comes from a much shorter pipe. And on the sun, that's telling us information about very close to the surface of the sun, not very deep at all into the sun.

NARRATOR: There are ten million different frequencies resonating in the sun. Deciphering them leads to a seismic shift in understanding its structure, creating a new science, "helioseismology."

TODD HOEKSEMA: Once the helioseismology came along, we could not only see what the surface was, but we can actually tell what the physical processes were underneath. So, by looking inside, we can actually see what the sun is doing.

NARRATOR: It is a powerful tool to see beneath the sun's surface. Studying the sun's sound waves reveals a complex, multi-layered machine. Directly beneath its blazing surface is a zone of perpetual churning. Next, is a layer where light takes thousands of years to cross. At the center, is the sun's core. It's the smallest region, but it's over 25 times the diameter of Earth. This is the powerhouse of our star. Everything we experience on Earth—sunlight, heat and the effects of solar storms—starts here.

So what's it like here? What is the core made of?

LUC PETERSON (Princeton Plasma Physics Laboratory): Well, the sun's a crazy place, right? It's far too hot to be a solid. We know that. Heat it up, it's far too hot to be a liquid. And so you think, well, it's a gas, right? Well, not really. It is this gaseous soup of charged particles that we call "plasma."

NARRATOR: You're more familiar with this soup than you might think.

LUC PETERSON: There are plenty of examples: fluorescent lightbulbs, flames, neon lights, perhaps fancy TVs that I can't afford, these are all plasma, plasma is sort of all around you.

NARRATOR: But plasma is radically hotter at the sun's core. The closest thing on Earth is lightning. During thunderstorms, electric charges build up, creating lightning bolts that reach tens of thousands of degrees.

LUC PETERSON: That's pretty hot, but it's nowhere near as hot as in the core of the sun. So, if you're going to travel into the core of the sun, the plasma would be 15-million degrees.

NARRATOR: As the sun formed, hydrogen gas at its heart was crushed under the weight of the material above. Eventually temperature and pressure rose so high, the hydrogen atoms broke apart into electrons and protons, creating plasma.

LUC PETERSON: It's under these extreme conditions that something really, really cool happens: nuclear fusion.

NARRATOR: It's the same atomic process inside the hydrogen bomb.

Under tremendous pressure, protons in the plasma fuse together, releasing photons, minuscule packets of heat and light. An unimaginable number of photons are made every second, generating the sun's incredible power, some of which reaches us as sunlight. This atomic alchemy converts over 4,000,000 tons of mass into energy, every second, in an endless loop.

LUC PETERSON: That much mass into energy is the equivalent of 10-billion hydrogen bombs being created every second. The sun does this day in, day out. It's been doing it for four-billion years, and it's going to continue to do so long after I'm gone.

NARRATOR: The energy of billions of bombs is released in the core every second. This begs a simple question.

LUC PETERSON: So you could ask, "Well, why doesn't sun doesn't blow itself apart?"

It's because there's this beautiful balancing act that occurs. In the core of the sun, you've got this pressure from all of this fusion pushing outwards, and the sun is huge, so you have all this gravitational pressure pushing downwards. And so, you have gravity pushing down and the sun trying to blow itself apart from the inside, and it is this beautiful balancing act between the two that keeps the sun in one piece.

NARRATOR: This light, born at the core, reaches us after a remarkable journey. Away from the core, pressure and temperatures drop, and nuclear fusion stops. Now, each photon begins a tedious journey through the sun's thickest layer of plasma, a region called the "radiative zone." Although squeezed less than at the sun's center, the plasma is still very dense, and photons struggle to move through it. Each packet of energy is continuously absorbed then spit out by the plasma particles.

TODD HOEKSEMA: In that particular part, there's no energy being generated, but the energy is transmitted by the radiation, so that's why we call it the radiative zone, not too surprisingly.

NARRATOR: The photons slowly bounce through the plasma here, ricocheting in a zig-zag path called the "random walk."

TODD HOEKSEMA: So, imagine that you're in a crowded room, and you're trying to make your way through, and you greet other people. And each person you greet, you have to say hello to, and then you move off in another direction.

So, it takes you a long time to get from one place in the room to another, because you are just kind of meandering your way around the room. So, the same way, the photons in the inside of the sun, they don't have a preferred direction, all they want to do is they want to be moving and they want to be greeting other particles.

NARRATOR: Though moving at the speed of light, 186,000 miles a second, it takes photons over 100,000 years to cross the zone. Eventually, the photons reach a boundary where pressures drop again, the plasma thins, and moving through it gets easier.

The photons still pack a lot of energy. Now they leak out into the convection zone, heating it from below. The thinner plasma in this zone makes the photons move in a different way.

TODD HOEKSEMA: So, instead of bouncing, all of a sudden there's an ordered motion. So, it's as if, all of a sudden, someone said, "Lunch," and all the particles decided, "Oh, we all have to go this direction." You still have to wait in line to get out, so it takes a month to get from the bottom of the convection zone to the surface, but it's a relatively short period.

NARRATOR: During this short period, heat from the photons sends plasma here into perpetual motion, a maelstrom of churning, 125,000 miles thick. Think of it like a massive lava lamp.

TODD HOEKSEMA: There's heat that enters at the bottom from the lightbulb. It heats the material and the blob rises to the surface. When it gets to the top, it cools off, and when it cools, it gets more dense and falls back down. This is a good analogy for what's happening inside the sun. We have the core of the sun heating the material at the bottom of the convection zone, material expands, and it carries the energy upward, until it gets to the surface.

NARRATOR: These incredible images reveal convection at the sun's surface, rising and sinking plasma, that creates a mesmerizing structure called granulation.

TODD HOEKSEMA: The granulation cells are about the size of the state of Texas. They only last for about 12 minutes, so there's an incredible amount of energy. It's a very dynamic, very chaotic place. And all of the activity is going on on the surface of the sun, where we can see it.

NARRATOR: Photons produced at the core finally reach the surface. They emerge as a weakened form of solar energy. This weakened energy reaches earth in eight minutes. We know it as sunlight.

TODD HOEKSEMA: So, a hundred thousand years, about a month, and then eight minutes. Once you get to the surface of the sun, it just takes eight minutes to get to where you can see it.

NARRATOR: Unimpeded, the trip from the core to the surface would take the photons a matter of seconds. In reality, the sunlight that shines on us today may have been created during the last ice age.



SOLAR DYNAMICS OBSERVATORY LAUNCH: Five, fourâ¦go for main engine startâ¦three, two, one, zero, and ignition and lift-off of the Atlas 5 with the Solar Dynamics Observatory.














NARRATOR: Back at the National Space Weather Prediction Center, Bill Murtagh tracks the storm's C.M.E. wave. It carries a billion tons of plasma, and it is now only about 20 hours from Earth.

What they see is alarming. It's not a single C.M.E. wave but one, two, three of them.

BILL MURTAGH: We won't call it the perfect storm yet, or anything, but conditions are lining up for some significant space weather.

NARRATOR: Their models show trajectory and speed, but the big unknown for Murtagh is how powerful the waves will be when they hit.

The answer lies in a force that governs the sun: magnetism. We're all familiar with magnets, they produce an invisible force that pushes and pulls on charged particles. In fact, Earth has a magnetic field that protects us against threats from the sun. But we are less familiar with the sun's magnetic power, which researchers believe plays a major role in driving solar storms.

KAREL SCHRIJVER: We've essentially learned that it takes two things to make a star magnetic. It needs to have these convective motions right underneath the surface: the bubbling of the gas; it needs to spin. And the faster it spins, the more active it becomes, and wherever those two things, the bubbling and the spinning, can interact, that's where we see the strongest magnetic activity in stars.

NARRATOR: Astronomers know that the surface of the sun spins in a strange way. Travel from the poles of the sun towards its equator and you'd notice it turns faster. Analyzing sound waves inside the sun reveals that the plasma layers beneath the surface also spin at different speeds. That's because they act like fluid, which gets denser towards the core. The interior of the sun is a place of spectacular turmoil, turmoil that's the key to the sun's magnetism.

TODD HOEKSEMA: The motions there, the convection, the differential rotation, the motion from equator to pole are driving a new force. They're driving a magnetic field. There's a dynamo at work here, a dynamo that's generating a force that we actually experience here on the earth.

NARRATOR: It works like a giant wind turbine: churning plasma in the convection zone stirs up powerful electrical currents, which generate a huge magnetic field.

NARRATOR: The Holy Grail for scientists is understanding exactly how this dynamo generates solar storms.

The clue lies deep within the convection zone. Magnetic field lines normally run from pole to pole, but with all the turmoil in the convection zone, that pattern can't last. Rotating layers stretch them horizontally, convection twists and braids them. Under immense strain, they begin to kink upwards towards the surface.

SARAH GIBSON: Imagine this spring is a magnetic field line. The magnetic field inside the sun is amplified, is strengthened by the rotating motions and the sheering motions and the churning motions inside the sun. It wants to expand upwards, and it does, until it pokes out through the surface of the sun.

NARRATOR: Tracking invisible field lines is normally impossible, but plasma plays a critical role.

SARAH GIBSON: Even though the magnetic field lines themselves are invisible, the plasma, which is heated and hot, can light up along these paths inâ¦maybe the same way as you could think of a highway, and at night you wouldn't see the highway at all, but with the cars with their headlights on, you'd see the path of the highway.

NARRATOR: Watching field lines is critical to understanding solar storms. As field lines emerge, they form loops. One end has a positive pole and the other a negative pole. Churning plasma beneath the surface twists these loops, pumping them with energy. If twisted enough, positive and negative parts of the loops cross. When they do, they short circuit, with a tremendous explosion. The energy released heats the plasma to millions of degrees, resulting in a spectacular solar flare. It's the final, dramatic stage of a very long journey.

Photons, formed in the core, make their way to the surface. Some pass directly into space as sunlight, but in the process, that surging energy disturbs the convection zone, generating a magnetic field. The field lines wind up, to the point that it explodes in a solar flare.

Now, S.D.O. provides a complete and unprecedented picture as these events evolve.

HOLLY GILBERT: This is beautiful, because the hot gas outlines the magnetic field lines that we would otherwise not be able to see, and here, you can see, even, a twisting structure, as some of the mass drains back down to the surface, and a lot of it escapes in the eruption. This is the essence of space weather or solar storms.

NARRATOR: This explains how flares form, but it's not the end of the story. Crossing magnetic field lines can cause nets of plasma to be flung into space. This is a coronal mass ejection, a C.M.E. wave. The portrait of how solar flares and C.M.E. waves form is coming into focus, but a key question remains. C.M.E. waves can travel 93-million miles to Earth in a matter of hours, so what gives them such explosive energy?

Part of the answer is hidden here, in the sun's atmosphere, the corona. It's made of superhot plasma that blisters at over 3,000,000 degrees Fahrenheit, 300 times hotter than the sun's surface. Some scientists suspect that this heat powers massive gusts of energy that blast C.M.E. waves toward Earth at incredible speeds, but why the corona is so hot is an enduring mystery.

SCOTT MCINTOSH: Understanding it's essential, if we want to get to the bottom of how the sun drives space weather and the impact of the sun on the earth.

NARRATOR: The fact that the corona is so much hotter than the surface flies in the face of physics.

SCOTT MCINTOSH: The sun's corona is very odd. Take this fire, for example. As I put my hands close, sure, it's warm, but as I pull them away, it gets cold. That's not the case on the sun at all. As you go in close, it's definitely warm, but as I pull away, it actually gets warmer still.

NARRATOR: Recently Japanese investigators observe high velocity jets of plasma, shooting up from the near surface. McIntosh suspects these jets deliver heat to the corona, but he doesn't have a way to confirm it visually, until he turns to S.D.O. for help.

SCOTT MCINTOSH: Lo and behold, we actually managed to join the dots and see, "Yeah, these objects that we could see moving out of the lower atmosphere at high speeds, kind of like these licks of flame, really were reaching a couple-million degrees. It was really a tumultuous moment. We kind of looked at each other and said, "Wow, what have we just done?"

NARRATOR: They've shown that the plasma jets, accelerating upwards from near the sun's surface, generate tremendous heat. As a result, temperatures in the corona soar to three-and-a-half-million degrees. If confirmed, it represents a huge leap forward in understanding C.M.E. behavior.

The immense heat of the corona acts like a wind in a raging gale. It's constantly pushing on the plasma draped on the field lines, billowing them out like sails pulling on a mast.

Like solar flares, when magnetic lines cross, there can be an immense explosion. In this case, the lines are cut, and the sail whips off into space. Loaded with a billion tons of highly charged plasma, the C.M.E. wave can wreak havoc on an electricity-dependent Earth.

At the National Center for Atmospheric Research, this violent event is captured by satellites.

SCOTT MCINTOSH: Now, to see the C.M.E., we need to create a little artificial eclipse. To do that, we block out the light from the disk of the sun, and that's this little circle, here. But what that allows us to do is see this extremely faint high-speed thing, shooting away from the sun. This one moves at about 1,000 kilometers per second.

NARRATOR: By enhancing the picture and slowing it down, it's possible to see the shockwave moving at over 2,000,000 miles per hour.

Though we have a better understanding of what causes solar storms and how they reach us, there is still a final pressing problem.

HOLLY GILBERT: Trying to predict when solar storms are going to occur on the sun really requires a lot of detective work. Basically we're looking for clues in observations to tell us when potential storms might occur.

NARRATOR: The best clue comes from these, sun spots, dark patches which can linger on the sun's surface for weeks at a time.

SARAH GIBSON: A sunspot is a massive region, several times the size of the earth, which appears on the sun as a dark spot. It's dark because it's relatively cool, compared to its surroundings, and it's cool because the magnetic fields are so strong that they're suppressing the flow of heat from below.

NARRATOR: The strong magnetic fields, which create sunspots, are the breeding ground for solar storms. The challenge is trying to decipher a pattern for when and how many will appear.

SARAH GIBSON: As we watch sunspots over a period of many years, we see something very interesting: the number of sunspots, at any given time, will wax and wane over a period of about 11 years. And since we now know that sunspots are associated with strong magnetic fields, this tells us that the sun's magnetic fields are, likewise, going through a cycle.

NARRATOR: The constant churning and twisting inside the sun creates a powerful dynamo, the biggest electrical generator in the solar system. The magnetic field lines it produces get so wound up that, roughly every eleven years, the magnetic poles of the sun reverse. After that, calmer magnetic activity prevails and fewer sunspots form, a period called "solar minimum." But because of the sun's turbulent nature, the field gradually winds up again. As it does, magnetic outbursts are far more common, a period called "solar maximum."

HOLLY GILBERT: The solar cycle actually determines the personality of the sun. During solar maximum, it can get very angry, and it can throw off solar storms that are sometimes directed at the earth. And during solar minimum, it becomes much more subdued. There aren't as many sunspots, there aren't as many solar storms occurring. The activity cycle basically determines how the sun is going to act.

NARRATOR: Prior to the solar storm of February 15, 2011, things were pretty quiet on the sun. But that outburst marks an ominous turning point: the sun's magnetic activity is winding up again, as it heads toward solar max.

Just a few days ago, Bill Murtagh and the team at the Space Weather Prediction Center witness the turn.

NARRATOR: It's now time to let the world know what it might expect.

BILL MURTAGH: In the next couple of minutes here, we are going to have to make a decision and make the prediction that this coronal mass ejection is going to arrive at whatever time tomorrow. And the geomagnetic storm will ensue, of course, once it arrives.

NARRATOR: Murtagh knows that the severity of the storm depends mainly on two things: how strong the C.M.E.'s magnetic field is and at what angle it hits Earth's own magnetic field.

C.M.E. waves approach Earth like a slowly rotating shield. One end is positively charged, the other negative. With magnetism, opposites attract and like poles repel. If the wave's positive pole lines up with the Earth's positive pole, most of power of the storm will be repulsed, but if opposite poles line up, the plasma the waves are carrying will hit with full force.

NARRATOR: Murtagh makes his final assessment only hours before impact.

NARRATOR: According to the observations, the C.M.E. wave will be repelled.

BILL MURTAGH: We don't expect it to be too strong. We'll see moderate storming levels, which is good enough to produce some aurora borealis down in the United States, along the Canadian border, the northern tier states. And it will cause some minor problems to the power grid and whatnot.

NARRATOR: This time, we dodged a bullet. But disturbing evidence suggests the earth will not always be so lucky.

It's a cautionary tale. NASA's Jim Green discovered it while researching a book on the American Civil War at the Library of Congress. Green found news accounts from 1859, which caught his eye.

JIM GREEN: I would run across articles about aurora, fabulous aurora. And this really piqued my interest, because it's in my field.

(Reading from news accounts) "It seemed as though the armies of heaven were engaged in terrific but noiseless conflict. This terrific aspect soon subsided into more beautiful and brilliant appearance, a few of which I can only refer to."

NARRATOR: On the day before the waves hit, a British astronomer observes a giant sunspot group light up with two massive flares. The second C.M.E. wave hit 18 hours later, allowing Green to calculate its speed—5,000,000 miles an hour—plowing into Earth at almost four times the speed of the February 15, 2011, C.M.E. waves.

Using the various reports, Green is able to reconstruct the 1859 storm. The accounts suggest that the poles of the C.M.E. waves were aligned, and instead of being repulsed, the waves hit with full power. The charged particles funnel down into the atmosphere, electrifying it like a giant neon sign, producing dazzling aurora displays. The storm is so intense, Earth's magnetic field all but collapses. Millions of tonnes of plasma spill towards the equator and a powerful electric surge pulses over the globe.

For the largely pre-electrified world, the moment passes with minimal damage. That might not be the case today.

JIM GREEN: It has the potential of knocking out power grids. And if it burns out transformers that are hard to replace, we may be without electricity in many areas for a very long period of time. There's only a few places that makes these 125 kilovolt transformers. It takes several months to make them, and if you burn out half of them, we're going to be shooting squirrels and chopping wood out the back yard for a long period of time, just to survive.

NARRATOR: Today's solar scientists believe it's not "if" but "when" the next big one will strike. With the next solar maximum due in 2013, it begs an all important question: "Can we predict when the next solar storm will hit?"






JIM GREEN: Maybe, and the reason why is we've learned so much about the sun. We're getting better at it, but we have a long way to go. And the more we look at some of these historic events, the more we get a deeper appreciation for what we need to know.

NARRATOR: Today we see the sun better than ever before. We are beginning to understand it from the inside out, but its unpredictable personality means there will always be uncertainty when living with a star.

Broadcast Credits


Duncan Copp
Sarah Kinsella
David Fairhead
Lance Lewman
Clive North
Kevin Meredith
Philip Sheppard
Peter Latona
Lipsync Post
Selina Kay
Nick Anderson
Tim Waller
Steve Cookman
Lisa McStay
European Southern Observatory
Hinode Mission
NASA Goddard Scientific Visualization Studio
NOAA Space Weather Prediction Center
Swedish 1-meter Solar Telescope, Royal Swedish Academy of Sciences
Ralph Seguin, Thomas Berger and Bart De Pontieu - Lockheed Martin
Luc Rouppe van der Voort and Mats Carlsson - University of Oslo
Vasco M. J. Henriques, Royal Swedish Academy of Sciences
Basilica of the National Shrine of the Immaculate Conception
Boulder County Parks and Open Space
David Hosansky, Mark Miesch, Matthias Rempel and the NCAR VisLab
Doug Biesecker and George Millward
Jacquelyn Hayes and Peter Latona
Karel Schrijver
Library of Congress and Roberta Goldblatt
Madhulika Guhathakurta
Patricia Wieser, Princeton Plasma Physics Laboratory
Philip Scherrer
Susan Hendrix
Camille Lamothe Moore
Eric Stalzer
Brett Reinke
Laura Beth Ward
Jonathan Sacks
John Bredar
yU + co.
Walter Werzowa
John Luker
Musikvergnuegen, Inc.
Ray Loring
Rob Morsberger
Michael H. Amundson
Spencer Gentry
The Caption Center
Karen Laverty
Eileen Campion Victoria Louie
Kate Becker
Kristen Sommerhalter
Linda Callahan
Sarah Erlandson
Scott Kardel, Esq.
Janice Flood
Susan Rosen
Rachel Connolly
Kristine Allington
Lauren Aguirre
Rebecca Nieto
Nathan Gunner
Linzy Emery
Elizabeth Benjes
Pamela Rosenstein
David Condon
Lisa Mirowitz
Laurie Cahalane
Evan Hadingham
Melanie Wallace
Howard Swartz
Alan Ritsko
Paula S. Apsell
A Production of NOVA and National Geographic Television in association with Duncan Copp Ltd
© 2012 NGHT, LLC and WGBH Educational Foundation
All Rights Reserved


(solar storm)
Courtesy NASA


Phillip Chamberlin
NASA Goddard Space Flight Center
Sarah Gibson
High Altitude Observatory
Holly Gilbert
NASA Goddard Space Flight Center
Jim Green
Dir., Planetary Science Div., NASA
Todd J. Hoeksema
Stanford University
Scott McIntosh
High Altitude Observatory
Bill Murtagh
Space Weather Prediction Center
Dean W. Pesnell
NASA Goddard Space Flight Center
Luc Peterson
Princeton Plasma Physics Lab
Karel Schrijver
Lockheed Martin


Full Program | 53:06

Full program available for streaming through

Watch Online
Full program available