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(Music: Gustav Holst:|"The Planets") In 1973, nine astronauts were|sent to live and work in the world's first|space station - Skylab. Their mission was|to observe the sun, free from the Earth's|distorting atmosphere. They witnessed what|no one had seen before, a sun more powerful|than they had ever imagined. To our ancestors, the sky was|a patchwork of puzzles. At night, it was brimming with|pinpoints of light - stars. Then there was the sun, whose arrival banished the stars|and brought warmth and light. It was hailed as the giver|of life, the first god. This is the story|of mankind's struggle to see behind the glare and|glimpse the truth about the sun and how we came to understand its power and|its role in the universe. (Carnival music) In February 1998, the Caribbean island|of Guadeloupe geared itself up|for a rare celestial event. For a few minutes,|day would become night during a total|eclipse of the sun. This was Francisco|Diego's tenth eclipse. As a boy, he was deeply|affected by his first. It started a lifelong|fascination with the sun. 'The sun was perceived|as an immaculate' gold disc, perfect. It was a religious belief. Everything was perfect|in the sky. The sun was|the most perfect circle, with no blemishes or structure. A perfect, flat, golden disc. 'It was the sun god|for many religions.' The sun remained|a symbol of perfection until a 17th-century|Florentine called Galileo first pointed|a telescope at the sky, and instantly recorded|the first scientific milestone. 'Galileo applied the|telescope for the first time, 'and discovered|the sun wasn't perfect. 'It had sunspots. 'That was a major revolution|in philosophy and science.' Galileo watched the sunspots move across the sun's surface... and realised it was spinning. It was the first of many|secrets sunspots would reveal. Galileo's insight|heightened speculation about the true|nature of our sun. But for two centuries, astronomers were frustrated|by its blinding disc. What were sunspots? What other landscapes|existed on the sun's surface? What was|the source of its power? There were moments,|scientists realised, when the sun offers a rare|and special opportunity. Roughly six times every decade, somewhere around the world, the sun passes|directly behind the Moon. If the sun's this big, Earth's a little ball|of 3-4mm in diameter and the Moon is even smaller. It's a quarter of the Earth, 400 times smaller than the sun. The fantastic coincidence is that the sun is|400 times further away than the Moon from us, so we see both more|or less the same size. (Man ) One minute! For 4 hours, Francisco watched the Moon|creep into position. (Man ) No filters! He came halfway round the world for just four minutes|of totality. But where the sun is concerned, dedication has never been|any guarantee of success. (People shout and cheer) Francisco got just a few moments|to glimpse the hidden sun. We lost it. No corona. Like many astronomers before|him, Francisco was thwarted as the clouds rolled in|to spoil the party. Douglas Gough is a|leading solar scientist. To see his first total eclipse,|he had travelled to Indonesia. The government had declared it|illegal to watch the eclipse, at least for the Indonesians. They had to watch it on TV or go to the mosque and pray the|dragon would spit the sun out. They believed|that was happening. I was standing on a road, and a little boy came up to me. I gave him a dark film,|to look at the sun. An old man of 70, the head of|the village, came too, and the three of us saw|a fantastic eclipse. A total eclipse|reveals the sun's corona, an outer layer|normally lost in the glare. 'An eerie feeling,|and almost total silence. 'The only thing we heard was|the chanting from the mosques.' This is what early astronomers|travelled the world to see. Within the corona|were seemingly burning clouds. The surface looked smothered in a complex, raging atmosphere. 'You realise,|seeing these things, 'the sun's active,|not a passive ball of gas. 'It's churning away. Interesting|things are happening.' Discovering new|things is exciting. That's why explorers explored|places no man had been before. On Earth, there's little left,|so we go into the universe. Seeing the sun,|peeling off a layer of mist, of lack of understanding,|and seeing how something works, is an amazing experience. The rarity of a clear eclipse gave scientists few chances|to study these prominences. In the 19th century,|Father Angelo Secchi, the Vatican's chief astronomer, caused a revolution|in the way we looked at light. From an observatory|above his church, he pioneered a new branch|of science - spectroscopy. His spectroscope split sunlight|into its constituent colours, then magnified|the light in one region. It was possible|to see the sun's edge, without relying on an eclipse. Spectroscopy revealed|a solar surface of astonishing complexity. You were no longer dazzled|by the sunlight. You could see the things you can see at the edge|of the sun during an eclipse. Soon astronomers were|studying the body of the sun. The sunspots were Earth-sized|tears in the surface. Like windows|on a mysterious interior. The surface itself|bubbled before their eyes. Soon they were cataloguing|the chemicals in the sun. Dark bands in its|spectrum meant hydrogen, calcium, iron. Astronomers discovered an alien|element, unknown on Earth. They named it after Helios,|the Greek sun god. Helium. When Secchi turned|his spectroscope to the stars, he made his most|profound discovery. He recognised|the pattern immediately. Their chemistry was|identical to the sun. One great mystery of|the heavens was resolved. Our sun was a star. The sun was a star,|and one realised it belonged to|the family of stars. 'Scientifically,|that's fantastic, 'as we want to know|what the universe is like. 'By studying the sun,|we study a typical star.' In the '40s we got|our first inkling of how deadly|a typical star can be. As the first rockets rose|to the fringes of space, they were scorched|with radiation. Our atmosphere lets|heat and light through, but shields us|from X-rays, gamma rays and ultra-violet|light from the sun. Soon a man was to brave|this deadly radiation, and come face to|face with a star. Alexei Leonov. 'Three, two, one, zero.' In 1973, a solar laboratory was sent to study|the sun directly from space. But the sun didn't|give up its secrets lightly. 'When Skylab was launched,|it had a heat shield, 'that was to open up|after it got into orbit.' Sixty seconds into flight, that heat shield popped open. It's still in the air stream, so the air stream|tore the heat shield off, and unlocked both solar wings. Conrad had been on the Moon when|he became crew leader on Skylab. Their home was no longer|protected by an atmosphere, and temperatures|started to soar. They had to find a way|of shielding the station from the sun's excesses. 'We got this|temporary heat shield rig, 'which we could rig from inside,|through an air lock.' We could push,|like an umbrella pole, and mylar sheets popped open|like an umbrella. 'Then we could pull it to where|it was offset a few inches. 'It did make the temperature|go down immediately.' As the temperatures dropped, the|crew went into the observatory. They had to get used to life|in a weightless environment. At first, nausea prevented all|but the most hardy from eating. That problem quickly passed.|Soon space didn't seem so bad. Then, with no distorting|atmosphere to blur their sights, the most extensive period of|solar observation ever began. 'The Skylab flight|is very dear to my heart.' I know a lot of people|don't understand that... It means more to me|than going to the Moon. Part of that was being able|to run the solar telescope and know we were bringing back a|tremendous amount of information that nobody had before|in great quantities. When I switch to the two|positions called h-alpha, these words stand|for hydrogen-alpha, called that|because the light here comes from light from hydrogen|atoms in the sun's atmosphere... Viewing the sun in the same|wavelengths of light used by Secchi|100 years earlier, the astronauts saw incredible|details on the sun's surface. ..wavelength radiated|by the hydrogen atoms. We can see sunspots,|networks, filaments, all of these things,|in great detail. We all took a four-hour turn|at the solar telescope panel. It's like playing|three 88-keyboard pianos at the same time. 'It was a very complicated set|of switching and everything.' It was very intense. You'd work hard to make sure the|sequences read the right way. Things would come up in real|time, like solar flares, so we had to be prepared|to catch that also. Solar flares are planet-sized|eruptions of boiling gas, prominences that|break free of the sun. They'd been seen from Earth, but|not in such detail and quantity. Somebody was running it and|would call us to take a look. That happened frequently, when something unusual came up|that we could witness, we'd call the other|guys up to take a peek. In nine months, successive Skylab crews took|more than 160,000 images, revealing hitherto|unknown aspects of the sun. Their most spectacular|discoveries were the coronal mass ejections, outbursts of material on a|scale that dwarfed solar flares. These were the best|views yet of the angry sun. But what causes|these convulsions? The answer lies in an|invisible side to our sun, and once again, sunspots|were the key to its discovery. Long before the space age, the summit|of the San Gabriel mountains was the closest an American|could get to space. In 1903, George Ellery Hale, the son of an engineer,|had a dream. He'd build the world's most|advanced solar observatory, high above the town of Pasadena. Sallie Baliunas|is an astrophysicist at the Mount Wilson observatory. Hale is my personal hero. He was a great scientist and|had instinct about engineering, so he could successfully build|the world's largest telescopes. He raised a lot of money|to do these projects. 'As he often said,|he made no small plans.' The route to the top of|Mount Wilson wasn't easy. 'This road wasn't built|until 1936, 'so all the concrete and steel|had to be brought up 'by backpack or mule train on|a very steep seven-mile trail.' The packhorses made 60 trips to|transport the telescope alone, but Hale soon had an observatory|that was the envy of the world. His first challenge was|to understand the sunspots. Hale built a spectrograph, which is here beneath|this table. 75 feet below is a grating, that disperses|the light of the sun into its energy components. The grating|would look like this, and would break the sunlight|into its different colours. In this spectrum are the|absorption lines of the gases. With his unique spectrograph, Hale started analysing|the sun's surface. He could take|photographs of sunspots in more detail|than anyone had before. During a routine study of the chemical absorption lines|of the sun's surface, he made a breakthrough. 'Looking at the|quieter part of the sun, 'he saw ordinary-looking|absorption lines. 'Then as the sunspot|rolled into the slit, 'the lines began|to broaden and split.' Hale saw the lines split apart|and recognised the phenomenon. Voilą, magnetic fields.|He could see it. June 1908. Hale had unravelled one|of the sun's greatest mysteries. Sunspots were caused|by magnetic distortion. These distortions|are 4,000 times greater than the Earth's magnetic field. They suppress|the upward surge of gases, cooling the surface|by 2000 degrees, and causing the dark spots. 'A sunspot on the surface 'is just a twisted|and kinked magnetic field, 'looped out of the surface.' This magnetogram shows|how the surface is speckled with positive and negative|lines of magnetic force. These tortured field lines|channel the sun's storms - eruptions of plasma,|exploding outwards for thousands of kilometres, before being dragged back|into its boiling surface. 'Coronal mass ejections,|prominences, 'all features on the sun's|surface are magnetic in nature.' In one of the coldest places|on Earth, 15 years before Hale started|his investigation into the sun, a Norwegian scientist|had drawn his own conclusions about the sun's magnetism. In a land where you|can't see the sun for months, he was convinced you|could feel its presence in one of the most|beautiful phenomena on Earth. 'It may be strange|to see why we're here, far to the north, in the|darkness, dealing with the sun. But here you see|the aurora, the Northern Lights. I really like to see the aurora. It's beautiful in many colours you don't see anywhere else. It really lights up the dark|days here in wintertime. 'Earlier, it was thought|the Northern Lights 'was the souls|of dead soldiers fighting.' (Whistling and humming) Norway is one of the best|places to study auroras. Truls Hansen monitors|the radioactivity high in the Earth's atmosphere. This area of research|goes back over a century. 100 years ago, Norway's|most famous scientist dedicated his life to the study|of atmospheric disturbances. His name was|Doctor Christian Birkeland. Birkeland was|brilliant, but a bit mad. You might see|that from his book. It contains not only theories|about particles and the aurora, but a lot of ideas. Some right, most wrong. One of them was Terrela,|which we see clearly here. A vacuum chamber|with a small globe, pretending the Earth inside it. 'We can also see Birkeland,|controlling the experiment.' This experiment artificially|created the Northern Lights. To protect his brain from|radiation, he always wore a fez. Birkeland's theories|about the origin of auroras stemmed from years|of dedicated study. Auroral activity is|particularly energetic after a period|of solar activity. Birkeland wanted to find|a mechanism to link the two. These are|the old magnetometers, which have been operating|for more than 100 years. They're still used|here and there. Birkeland used|very similar instruments. Here's a recording|of the magnetic field, taken with this instrument. It starts quiet around noon, and then, here in the evening, you get a magnetic storm, which you see clearly here. During this period you have|a large and very bright aurora. This is the|Birkeland Terella experiment. He built several,|but this is the biggest one, and the last one,|I suppose, being made in 1913. It's a large vacuum chamber with|a model of the Earth inside. Birkeland thought the magnetic|storms with the Northern Lights were caused by|electrically-charged particles buffeting the Earth's|magnetic field. He believed these particles|came from the sun, but his ideas|were never taken up. In 1917,|Birkeland committed suicide. In fact, evidence of the|extraordinary reach of the sun had been visiting|our skies for millennia. The dusty comet tails always|point away from the sun. It was assumed that|sunlight alone was the cause. But in 1947, a German physicist,|Ludwig Bierman, calculated that something|far more substantial had to be pushing|the comet tails. He called it|solar corpuscular radiation, and his idea|was rejected immediately. Despite the general derision,|physicist Eugene Parker was unable to dismiss|Bierman's argument. 'I had a chance|to talk to him in Chicago.' He said if it isn't sunlight, then it must be|the solar corpuscular radiation, the emission|of particles from the sun that blow the tail away|from the sun. 'His revelations made me see|he had a fundamental point.' The physicist Sidney Chapman was|very eager to attack Bierman. He said the sun was 330,000|times more massive than Earth, and that no particle,|however small, could escape|its enormous gravitational pull. Regardless of his scorn|for the solar wind, Chapman was developing|his own idea for how the sun was|reaching out to the Earth. He suggested the corona, though firmly bound to the sun, stretched much farther|than is seen during an eclipse. Eugene Parker met Sidney Chapman|in Boulder, Colorado. I was thinking about what|I had learned from Chapman, that the corona extends out|through the solar system. I realised that Chapman and|Bierman were mutually exclusive. The solar corpuscular radiation|that affects the comet tails can't penetrate through a static|corona, interactions block this. But I could not see that|either one of them was wrong. Parker worked at the apparent|contradiction in the theories, and found that both were right. 'I integrated|the equations of motion.' I found only one solution|that fitted the condition of strong rebound at the sun|and zero pressure in infinity. That was the solution providing|the supersonic solar wind. Parker's solar wind was more|complex than Bierman's version. He calculated the corona|did have enough thermal energy to escape its gravity and|stream off at 500km a second. But when he went public,|Parker himself was ridiculed. 'The referees for my|papers were anonymous. 'I was assured|they were experts. 'They declared|the ideas were absurd.' Others declared it was false, and published papers|showing alternatives, and gave lectures|decrying the idea. My friends said,|"It was a great idea, "but great ideas often|fall on their face." My reaction was, "We'll see|what falls on its face." Parker waited five years|for his theory to be vindicated. in 1962, the Mariner 2 probe to|Venus carried particle detectors designed to discover|how empty space was. The world's first interplanetary|probe signalled back that space is awash with a solar wind|exceeding Parker's estimates. 'The JPL plasma detector 'showed there was a wind 'of anywhere from 300|to 800km per second.' The wind was always|there and never ceased. I refused to argue|with anybody after that. Modern telescopes|have revealed the complexity of Parker's solar wind. From the sun's equator particles|constantly evaporate into space. Occasionally, gusts break free of the sun's gravitational|and magnetic forces. These are the flares and coronal|mass ejections seen by Skylab. These electrically-charged|hurricanes are ferocious and relentless. The planets lie|in their firing line. Mercury, closest to the sun, bares the brunt|of the solar wind. Any atmosphere this world may|have had has been blown away, leaving its surface|bathed in deadly radiation. Mars is four times further|from the sun than Mercury, yet it's thought|the solar wind has stripped a third of its|original atmosphere, leaving a veil one hundred|times thinner than ours. Venus, our nearest neighbour, has an atmosphere a|hundred times thicker than ours. Modern probes|discovered a comet-like tail that stretches back|to the Earth's orbit. The clouds on Venus are also|being eroded by the solar wind. And what of our atmosphere? Earth has a magnetic field that|stretches far out into space. It deflects the solar wind|and protects our atmosphere. A force-field fighting|a constant battle with the sun. The solar wind and the Earth's|magnetic field battle together. The magnetic field is being|compressed by the solar wind. 'As this pressure increases, 'and sends the particles through|along the magnetic fields 'down to the|Earth's polar areas, 'we see them as aurora|in the upper atmosphere.' We live in a region|dominated by the solar wind, which extends|far out into space. 'The next question is how far|out into space it extends, 'as it spreads out|farther from the sun.' What is the full|extent of the sun? The first space|probes venturing to Jupiter recorded massive|radio emissions. That was the same battle between Jupiter's magnetic|field and the solar wind. As the spacecraft Voyager|visited the outer planets, it found the same|signature of solar wind buffeting magnetic fields. When it left Neptune,|the solar wind was still there. Where would it end? Three years beyond Pluto, it detected a mysterious|burst of radio energy. The signals were picked up at the tracking station|at Goldstone, California, where Don Gurnett had been|keeping in touch with Voyager. My primary interest now|is following the solar wind as it expands out from the sun. It has to be stopped some|place by the interstellar gas. This boundary|we call the heliopause. The radio burst picked up by|Voyager was totally unexpected. There were no giant planets|within three billion kilometres. We didn't know|the signal's origin. We thought it was coming|from Jupiter or Saturn. Or maybe it was coming from|much further away from the sun. Their search led them back to|the heart of the solar system. We noticed a series of very|powerful coronal mass ejections, 'some 400 days|before the radio burst.' Checking|through Voyager's log, Don found it had been overtaken|by the outburst after 100 days. 300 days later, the solar gust|reached a magnetic boundary. Was this the heliopause, the|outer limit of the solar wind? Our model is that|this coronal mass ejection produced a plasma pulse|coming out from the sun that propagated for 400 days. We detected it|going by Voyager One and Two. That pulse of plasma eventually|reached the heliopause, and caused the radio emission. The radio burst|places the heliopause at four times|the distance of Pluto. This is the extent of the sun. Even the most distant planets, where the sun's|just a bright star, bathe in its|evaporating atmosphere. The planets are bound|by our sun's gravity. They were formed as|a by-product of its creation. There's a more fundamental bond between the planets|and the stars. The very stuff of life|is built inside them. A star's core is|the ultimate fusion reactor. Douglas Gough wants|to see it in action. 'My goal is to learn about|the structure of the core, 'because the nuclear physics|is so interesting.' The nuclear reactions|that change material, that produce new|particles that leave the sun, help us understand the physics|of elementary matter. 1995 saw the launch of a|new era of solar exploration. A journey that may take us to|the heart of a star. The solar observatory SOHO|can view the sun in X-rays, ultra-violet and visible light. But SOHO doesn't|just look. It listens. In 1975, when Gough learned the sun's|surface rippled like a pond, he instantly saw|a way to see to its core. 'I realised this is a way|of seeing inside the sun.' You can't see inside the|sun with light, it's opaque. But this was sound.|You can hear inside it. By doing so, you could learn|the structure of the sun inside. I found that an amazing concept, that you could|get inside a star. The surface of|the sun is heaving. Every six minutes the entire|star breathes in and out. Its gaseous ocean|swells and dips, and a complex pattern of ripples|shimmer across its surface. Clues to the structure within. 'The sun's like|a chorus of instruments, 'playing, but not in tune.' It's cacophonous, which gives much information|about the detailed interior. The sound waves|move back and forth, and give tones,|like a musical instrument. SOHO has revealed|new surface phenomena. After a solar flare,|seismic quakes spread out for thousands of kilometres.|But there's much more. 'We've learned|about the sun's outside' from studying the|sound waves from SOHO. We've learned about the dynamics|and the chemical composition. We want to do something|similar in the core. SOHO has started to strip|away the sun's outer layers. Under its surface, it|discovered rivers of plasma, super-heated gases|that circle its pole. Looking like the|jet stream on Earth, it seems the sun|has weather too. But deep in the core is that|remarkable chemical factory. 'The stars make all|the matter that we are made of, 'from hydrogen and helium.|That's what we're made of. 'They're the factories|that make material. 'To understand the universe,|we need to study the stars.' Every star has a core. Almost all stars are|generating nuclear energy, transmuting elements|from one to another, building up the heavy|elements of the universe. We believe the stars' physics|are the same as on Earth. This physics we must|understand more carefully, so we can work out|what that implies about the structure of the|universe and how it evolves. In the beginning, the universe|contained hydrogen and helium. For 12 billion years, stars|have been transforming them into more complex elements. Our sun is born|from that process. 4.5 billion years ago, a star on the fringes|of our galaxy ended its existence|as a supernova. Its death throes sent the|contents of its core into space. These heated grains of silicon,|iron and many other elements careered into a cloud of gas,|causing it to collapse. As the gas and dust mixture|went to the cloud's centre, they ignited a nuclear reaction|and our sun burst into life. The remaining debris from the|supernova formed the planets. We are made of star dust,|forged in the heart of a star. In the last 400 years, science has peeled back|our sun's layers, to reveal a star, one of the|countless engines of creation, which made the planets,|which made us. Our ancestors saw a|perfect disc of light. A god. Science has revealed|an entity more powerful |
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