Planets The 5 - Star
(Music: Gustav Holst:|"The Planets")
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 -
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.
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.
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,
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.
'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.
'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.
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.
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
P S 2004
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Police Story (2004) CD1
Police Story (2004) CD2
Police Story 2
Poltergeist 2 The Other Side 1986
Poltergeist 3 (1988)
Pork Chop Hill
Porky - Awful Orphan (1949)
Porky - Dough for the Do Do (1949)
Porky - Porky Chops (1949)
Porky - The Wearing of the Grin (1951)
Pornostar (Poruno Suta)
Port of Call (1948)
Portrait of a Lady The
Poseidon Adventure The
Poslusne hlasim (1957)
Possible Loves - Eng - 2000
Post Coitum 2004
Postman Blues (1997)
Power Play (2002)
Presidents Analyst The (1967)
Prick Up Your Ears
Pride and Prejudice
Pride and Prejudice CD1
Pride and Prejudice CD2
Pride and Prejudice CD3
Pride and Prejudice CD4
Pride and Prejudice CD5
Pride and Prejudice CD6
Pride and Prejudice The Making of
Pride and the Passion The
Prime of Miss Jean Brodie The CD1
Prime of Miss Jean Brodie The CD2
Prince and the Showgirl The
Princess Blade The
Princess Bride The
Princess Diaries The CD1
Princess Diaries The CD2
Princess Of Thieves
Princess and the Warrior The
Prisoner of Second Avenue The
Private Life of Sherlock Holmes The (1970)
Project A CD1
Project A CD2
Psycho - Collectors Edition
Public Enemy (2002 Korean) CD1
Public Enemy (2002 Korean) CD2
Public Enemy The
Pulp Fiction (1984)
Pump Up The Volume
Pumping Iron (1977)
Punisher The (2004)
Punisher The 1989
Pupendo (2003) CD1
Pupendo (2003) CD2
Purple Rose Of Cairo The
Purple Sunset (2001)
Pusong Mamon CD1
Pusong Mamon CD2