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ROWE: White dwarfs,
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small stars that pack
a big punch.
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When white dwarfs
were first discovered,
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astronomers' reaction
was no, no, no, no,
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no, no, no, that can't be real.
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BULLOCK: What's going on
inside these things
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can only be described
as seriously weird.
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ROWE: They're the cooling
corpses of stars
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like our sun,
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but new research proves
white dwarfs are
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one of the driving forces of
our universe.
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PLAIT: They eat planets, they
flare out in high-energy light.
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They can really explode.
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And they can tell us literally
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about the nature of
the universe itself.
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NARRATOR:
And there's a dirty secret at
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the heart of
white dwarf science.
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HOPKINS:
We see dead stars exploding,
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and we still don't understand
why they're doing it.
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ROWE: Have scientists finally
discovered how these small
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stars could be such massive
galactic players?
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[explosion blasts]
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December 2018.
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Astronomers spot
strange flares coming from
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a galaxy 250 million
light-years from Earth,
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GSN 069.
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We know that GSN 069 has
a supermassive black hole in
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its center, equal to about
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half a million
times the mass of the sun.
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That's a big black hole,
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and it blasts out X-rays in
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a very, very steady pace,
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every nine hours. Why?
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ROWE: The flares are
so energetic and regular,
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the supermassive black hole
must be eating the mass of
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the planet Mercury
three times a day.
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The big question is what's
feeding this black hole
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such a huge dinner?
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ROWE: In March 2020,
scientists found the answer.
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An unlucky star at the end of
its life
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had wandered into the death
zone of the black hole.
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OLUSEYI: A star getting
too close to a supermassive
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black hole is like
a glazed doughnut
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getting too close to me.
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That thing just is not
gonna make it.
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HOPKINS: Stars to get too close
to a black hole
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get torn apart.
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They sort of get attacked
by the black hole,
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and some of that material
is also getting launched
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off in very powerful winds
and jets and streams
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getting out.
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ROWE: Somehow, the star
survives its close
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encounter with
the supermassive black hole.
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Further investigation reveals
it's a small, compact star,
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a white dwarf.
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So what makes this tiny star
almost indestructible?
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The answer lies in how
it's formed.
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We get a clue if we look at
the life cycle of a star.
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It's burning hydrogen into
helium, that's causing nuclear
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fusion, and that causes a star
to stay stable.
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There's this delicate balance
between radiation pressure
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from that nuclear fusion pushing
out and gravitational pressure
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pulling in.
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But when stars like our sun
near the end of their life,
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they run out of hydrogen fuel.
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ROWE: The sun-like star makes
more and more helium,
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which builds up in its center.
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Gradually, the immense weight of
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the star's outer layers crushes
the helium core.
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OLUSEYI: As the core ages,
it gets smaller and hotter,
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which increases the rate of
nuclear reactions.
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ROWE: These nuclear fusion
reactions produce more energy,
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which pushes the outer layer,
or envelope, outwards.
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Because there's more energy
flowing through the envelope,
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the envelope swells up.
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ROWE: The star expands to around
100 times its original size.
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The yellow star
becomes a red giant.
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Eventually, red giants shed
their outer layers,
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forming stunning gas shells
called planetary nebulas.
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Planetary nebulae are the most
beautiful objects in space.
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They're all spectacular.
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A star that ends its life in
one of these planetary nebulas
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leaves behind a white dwarf
at the center,
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and this white dwarf is
essentially a cinder,
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a stellar cinder.
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It's what's left after
nuclear fusion
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is no longer possible for that
particular star.
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ROWE: All that remains,
a glowing white dwarf,
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the leftover core
of the dead star.
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But in galaxy GSN 069,
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the supermassive black hole
turbocharged the process.
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It stripped off the outer
layers of the red giant
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in a matter of days.
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HOPKINS: The black hole
has almost eaten
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all the juicy parts,
all the easy-to-get-at parts
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of star, leaving behind
the sort of
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bone or the leftovers
of the white dwarf.
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ROWE:
This white dwarf is just 1/5
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of the mass of the sun.
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00:05:06,172 --> 00:05:08,573
How can such a small
star survive
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being so close to a black hole?
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PLAIT: You might think that
because a white dwarf is small,
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it's not gonna last very long,
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because there's not that much
stuff there to eat,
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but it turns out
it's quite the opposite.
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ROWE: The pocket-sized white
dwarf is packed full of matter.
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If it were a normal star,
it would have been shredded
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long ago,
but because it's such a dense,
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tight ball of matter,
it survives.
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Imagine taking the sun
and crushing it down
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to just about the size
of the Earth.
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Same mass, but now packed way
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more tightly,
so a basketball-worth of this
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stuff would weigh as much
as 35 blue whales.
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ROWE: The white dwarf's extreme
density protects it from
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the gravitational onslaught of
the supermassive black hole.
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Its orbit takes it near that
black hole every nine hours,
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and every time it encounters
the black hole, some of its
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material gets sipped off.
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00:06:09,235 --> 00:06:10,702
They're playing a game
of interstellar
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tug of war with one another.
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The black hole is bigger,
so it's going to win.
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But the white dwarf is very
dense, so it's very tough,
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and it's able to hang in there
for quite a long time.
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OLUSEYI: It's gonna stay
in orbit around
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a supermassive black hole for
billions of years.
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Talk about David and Goliath.
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ROWE: When astronomers first
discovered white dwarfs,
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they thought
they shouldn't exist.
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How could something have
such an extreme density
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and not collapse under
its own weight?
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00:06:41,000 --> 00:06:43,535
Quantum mechanics,
the science of atomic
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00:06:43,636 --> 00:06:46,571
and subatomic particles
has the answer.
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SUTTER: We're used to the rules
of physics up here
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in the macroscopic world,
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but when you zoom down into
the subatomic world,
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things get weird.
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Here we have the electron,
one of the tiniest
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00:07:00,987 --> 00:07:02,587
particles in the universe,
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00:07:02,688 --> 00:07:05,891
and it's these little
electrons that are doing
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the work of supporting
an entire star.
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Electrons really don't like
being squashed
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into a small space.
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If you try to squash too many
of them into too small a space,
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they'll push back really hard,
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and this is an effect
called degeneracy pressure.
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ROWE: These degenerate
electrons stop white dwarfs
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from collapsing,
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but they give these stars
strange qualities.
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OLUSEYI: White dwarfs behave
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very differently
than normal matter.
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Take planets and stars.
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They become bigger
when they gain mass.
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White dwarfs
are the exact opposite.
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As they gain mass,
they get smaller.
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ROWE: The more massive
a white dwarf,
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the tighter the electrons
squeeze together,
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and the smaller and denser
the star gets.
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The high density means
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the white dwarf's structure
is also strange.
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It has an extremely
thin atmosphere,
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made of hydrogen
or, occasionally, helium gas.
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If you were to take an Earth
skyscraper and put it on
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a white dwarf star,
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if you climb to the top of
that skyscraper,
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you'd be outside of the white
dwarf's atmosphere.
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You'd actually be in space.
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ROWE: Beneath the thin
atmosphere lies a surface
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of dense helium
around 30 miles thick.
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It surrounds an interior made
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of superheated liquid carbon
and oxygen.
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A white dwarf at its surface
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can be a half a million degrees.
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It's even hotter in
the interior,
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and so that kind of material,
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it's not gonna behave
the way normal matter does.
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ROWE: Eventually,
over billions of years,
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the center of the white dwarf
cools down into a solid.
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CHRISTIANSEN: As the carbon
and oxygen atoms cool down,
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they form a crystal.
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Diamonds are actually crystals
of carbon,
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so at the center of
these cool white dwarfs
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could be a diamond the size
of the Earth.
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ROWE: White dwarfs gradually
give off their remaining energy
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until there's just a cold,
dead ball of matter,
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a black dwarf.
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00:09:08,748 --> 00:09:11,016
HOPKINS: We've never seen what
we call a black dwarf,
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00:09:11,117 --> 00:09:12,717
and there's a simple reason
for that.
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00:09:12,818 --> 00:09:14,920
It takes a tremendous amount
of time,
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many tens of billions of years,
longer than the age of
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the universe,
to reach that point.
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ROWE: This is the dark destiny
of most midsized stars,
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including our sun.
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00:09:26,866 --> 00:09:31,136
This long, slow death may make
white dwarfs seem ordinary,
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00:09:32,505 --> 00:09:34,406
but these tiny stars
could answer
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some big questions
about our universe.
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PONTZEN: They might be small,
and they might be dim,
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00:09:41,213 --> 00:09:44,849
but they are essential for
our understanding of physics.
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ROWE: New research into
white dwarfs may answer
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00:09:48,955 --> 00:09:50,689
one of the biggest questions
of all...
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00:09:50,790 --> 00:09:54,125
Can life survive the death
of its star?
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00:10:05,871 --> 00:10:07,739
ROWE: In the past,
we've underestimated
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00:10:07,840 --> 00:10:09,407
white dwarfs,
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00:10:09,508 --> 00:10:13,578
but now they're causing
a buzz among astronomers.
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00:10:13,679 --> 00:10:15,680
One of the big questions
over the last
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00:10:15,781 --> 00:10:20,852
decade is could a planet
survive around a white dwarf?
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00:10:20,953 --> 00:10:22,754
The logical answer would be no.
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00:10:22,855 --> 00:10:24,456
On their way to becoming
white dwarfs,
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00:10:24,557 --> 00:10:26,825
stars evolve through
a red giant phase.
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00:10:31,097 --> 00:10:33,198
They expand to become very huge.
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00:10:35,334 --> 00:10:36,568
So we figured any planets around
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00:10:36,669 --> 00:10:39,070
these stars might just
get eaten.
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00:10:42,775 --> 00:10:46,745
ROWE: In December of 2019,
evidence from the constellation
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00:10:46,846 --> 00:10:49,681
of Cancer turned that idea
on its head.
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00:10:49,782 --> 00:10:54,119
Astronomers spotted
a strange-looking white dwarf
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00:10:54,220 --> 00:10:56,821
about 1,500 light-years
from Earth.
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00:11:00,159 --> 00:11:02,727
Subtle variations in light
from the star
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00:11:02,828 --> 00:11:04,729
revealed a mystery...
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00:11:04,830 --> 00:11:08,466
The elements oxygen and sulfur
in amounts never
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00:11:08,567 --> 00:11:12,070
before seen on the surface of
a white dwarf.
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00:11:12,171 --> 00:11:14,572
We know what the chemical
signature of a white dwarf is,
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00:11:14,674 --> 00:11:16,107
and this stuck out
like a sore thumb.
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00:11:17,476 --> 00:11:19,511
ROWE:
Normally, hydrogen and helium
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00:11:19,612 --> 00:11:22,113
make up the outer layers
of a white dwarf.
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00:11:22,214 --> 00:11:23,381
Oxygen and sulfur
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00:11:23,482 --> 00:11:25,050
are heavier than hydrogen
and helium,
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00:11:25,151 --> 00:11:27,152
and they should have sunk
down, but we still see them
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00:11:27,253 --> 00:11:30,689
there, so they must have
gotten there recently.
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00:11:30,790 --> 00:11:33,725
ROWE: Using ESO's Very Large
Telescope in Chile,
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00:11:33,826 --> 00:11:37,395
astronomers took a closer look.
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00:11:37,496 --> 00:11:40,298
They discovered a small,
Earth-sized white dwarf
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00:11:40,366 --> 00:11:43,601
surrounded by a huge gas disc
roughly 10 times
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00:11:43,703 --> 00:11:45,637
the width of the sun.
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00:11:45,771 --> 00:11:48,973
The disc contained hydrogen,
oxygen, and sulfur.
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00:11:49,075 --> 00:11:52,444
SHIELDS: A system like this had
never been seen before,
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00:11:52,545 --> 00:11:55,213
and so the next step was to
look at a profile of these
237
00:11:55,314 --> 00:11:57,082
elements and figure out where
238
00:11:57,183 --> 00:11:58,950
we'd seen something similar.
239
00:11:59,051 --> 00:12:02,821
And the amazing thing is,
we have.
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00:12:02,922 --> 00:12:06,991
We've seen these elements in
the deeper layers of the ice
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00:12:07,093 --> 00:12:08,860
giants of our solar system,
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00:12:08,961 --> 00:12:10,528
Uranus and Neptune.
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00:12:12,431 --> 00:12:14,899
ROWE: Hidden in the gas ring
is a giant,
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00:12:15,000 --> 00:12:17,402
Neptune-like icy planet.
245
00:12:17,503 --> 00:12:19,971
It's twice as large as the star,
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00:12:20,072 --> 00:12:24,109
but the fierce 50,000-degree
heat from the white dwarf is
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00:12:24,210 --> 00:12:26,578
slowly evaporating
this orbiting planet.
248
00:12:26,679 --> 00:12:28,246
SHIELDS: The white dwarf
249
00:12:28,347 --> 00:12:32,050
is bombarding the planet with
high-energy radiation, X-rays,
250
00:12:32,151 --> 00:12:33,218
UV rays.
251
00:12:33,319 --> 00:12:36,087
It's pulverizing the ice
molecules in its atmosphere
252
00:12:36,188 --> 00:12:38,189
and blowing them out into space,
253
00:12:38,290 --> 00:12:40,291
and the ice molecules are
streaming behind
254
00:12:40,392 --> 00:12:42,293
the planet like
the tail of a comet.
255
00:12:42,394 --> 00:12:45,230
ROWE:
The icy planet loses mass at
256
00:12:45,331 --> 00:12:49,033
a rate of over 500,000 tons
per second.
257
00:12:49,135 --> 00:12:52,670
That's the equivalent of
300 aircraft carriers
258
00:12:52,772 --> 00:12:55,240
every minute.
- CHRISTIANSEN: It sounds like
259
00:12:55,341 --> 00:12:56,741
that could be curtains
for the planet.
260
00:12:56,842 --> 00:12:59,177
But remember,
the planet is large,
261
00:12:59,278 --> 00:13:02,247
and the star is cooling down.
- SHIELDS: As it cools,
262
00:13:02,348 --> 00:13:04,983
it will stop blasting
the planet so intently,
263
00:13:05,084 --> 00:13:07,018
and that stream of
gas will cease.
264
00:13:07,119 --> 00:13:08,686
The planet will probably
end up losing
265
00:13:08,788 --> 00:13:11,723
only a few percent of
its total mass.
266
00:13:11,824 --> 00:13:13,491
ROWE:
So the planet should survive
267
00:13:13,592 --> 00:13:16,828
and continue orbiting
the white dwarf.
268
00:13:16,929 --> 00:13:18,897
But a mystery remains.
269
00:13:18,998 --> 00:13:22,066
Why didn't the closely
orbiting planet die
270
00:13:22,168 --> 00:13:25,670
when the star swelled
to a red giant?
271
00:13:25,771 --> 00:13:30,775
SHIELDS: It had to have started
farther out and moved inwards.
272
00:13:30,876 --> 00:13:34,145
Our best guess is that other
ice giants were probably
273
00:13:34,246 --> 00:13:36,314
lurking somewhere
in the outer regions
274
00:13:36,415 --> 00:13:39,050
of the system and knocked
that planet inwards,
275
00:13:39,151 --> 00:13:42,120
towards the white dwarf,
sometime after the red giant
276
00:13:42,221 --> 00:13:45,390
phase in some kind of
cosmic pool game,
277
00:13:45,491 --> 00:13:46,591
if you will.
278
00:13:47,693 --> 00:13:50,428
ROWE: This isn't the only white
dwarf with evidence of planets.
279
00:13:50,529 --> 00:13:54,032
About 570 light-years
from Earth,
280
00:13:54,133 --> 00:13:59,671
there's a white dwarf star
called WD 1145+017.
281
00:14:01,807 --> 00:14:04,209
After studying the star
for five years,
282
00:14:04,310 --> 00:14:08,046
researchers report that
the white dwarf is ripping apart
283
00:14:08,147 --> 00:14:11,316
and eating a mini rocky planet.
284
00:14:11,417 --> 00:14:13,218
CHRISTIANSEN: So as the planet
is being torn up,
285
00:14:13,319 --> 00:14:16,221
we see this huge cloud of
dust blocking out 50% of
286
00:14:16,322 --> 00:14:18,623
the light of the star
and huge chunks of rock
287
00:14:18,724 --> 00:14:20,625
passing in front of the star.
288
00:14:20,726 --> 00:14:24,262
BYWATERS: It's exciting to see
this planet being torn apart,
289
00:14:24,363 --> 00:14:27,532
because it's not often
that we get to see an event,
290
00:14:27,633 --> 00:14:29,734
we get to see something
in the process
291
00:14:29,835 --> 00:14:32,003
that we can observe
and we can learn from.
292
00:14:34,773 --> 00:14:36,341
ROWE:
There's more and more evidence
293
00:14:36,442 --> 00:14:38,409
that planetary systems
can survive
294
00:14:38,510 --> 00:14:42,881
the death of their star and
the formation of a white dwarf.
295
00:14:42,982 --> 00:14:45,884
It just depends on
the planet's composition
296
00:14:45,985 --> 00:14:47,352
and location.
297
00:14:47,453 --> 00:14:51,589
The distance from the planet to
the star is a critical factor,
298
00:14:51,690 --> 00:14:55,460
because as you move farther
and farther out from a star,
299
00:14:55,561 --> 00:14:59,597
the intensity of that solar
radiation decreases.
300
00:14:59,698 --> 00:15:02,667
So the farther you go out,
the less heat you have,
301
00:15:02,768 --> 00:15:05,536
the less high-energy particles
are reaching the surface of
302
00:15:05,638 --> 00:15:07,372
that planet.
303
00:15:07,473 --> 00:15:11,075
Also, rocky planets can
survive better than gas giants,
304
00:15:11,176 --> 00:15:13,311
because rocky planets can hold
onto their stuff better,
305
00:15:13,412 --> 00:15:15,647
whereas gas can be blown
away much more easily.
306
00:15:17,816 --> 00:15:19,083
ROWE:
These new discoveries raise
307
00:15:19,184 --> 00:15:21,920
questions about habitability
around stars.
308
00:15:23,389 --> 00:15:26,824
Could white dwarf systems
support life?
309
00:15:26,892 --> 00:15:28,960
SHIELDS: If we limit
ourselves to only looking
310
00:15:29,061 --> 00:15:31,896
for life on planets
orbiting stars like our sun,
311
00:15:31,997 --> 00:15:35,199
we would be doing ourselves
a huge disservice.
312
00:15:35,267 --> 00:15:39,070
Far more important is to look
for, around whatever star,
313
00:15:39,171 --> 00:15:40,872
the habitable zone,
314
00:15:40,973 --> 00:15:43,875
the Goldilocks zone,
the region around a star where
315
00:15:43,976 --> 00:15:46,511
a planet could support life.
316
00:15:48,280 --> 00:15:50,148
ROWE: When it comes to
supporting life,
317
00:15:50,249 --> 00:15:53,918
white dwarfs have some
surprising advantages.
318
00:15:54,019 --> 00:15:55,920
CHRISTIANSEN: Even though
there's no fusion happening,
319
00:15:56,021 --> 00:15:58,423
they have all of this internal
energy stored up that they
320
00:15:58,524 --> 00:16:01,459
release that warms
the nearby planets.
321
00:16:01,560 --> 00:16:04,762
SUTTER: Life might even prefer
hanging out around
322
00:16:04,863 --> 00:16:06,264
a white dwarf, because
323
00:16:06,365 --> 00:16:08,533
it doesn't change much over
the course
324
00:16:08,634 --> 00:16:10,168
of billions of years.
325
00:16:10,269 --> 00:16:13,705
With something like our sun,
there are flares and coronal
326
00:16:13,806 --> 00:16:16,240
mass ejections, and then
eventually, it's gonna die,
327
00:16:16,342 --> 00:16:17,942
and we have to deal with that.
328
00:16:18,043 --> 00:16:19,844
That's not a problem with
a white dwarf.
329
00:16:21,113 --> 00:16:23,748
So if life can gain a foothold,
330
00:16:23,849 --> 00:16:25,883
it has a nice, stable home.
331
00:16:27,953 --> 00:16:30,888
ROWE: We now think 25 to 50% of
332
00:16:30,990 --> 00:16:33,558
white dwarfs
have planetary systems.
333
00:16:33,659 --> 00:16:36,094
Perhaps one day,
we'll find one with
334
00:16:36,195 --> 00:16:40,331
an Earth-like planet,
and maybe even life.
335
00:16:42,067 --> 00:16:45,003
But not all of these tough
little stars are good hosts.
336
00:16:46,472 --> 00:16:49,674
White dwarfs
have a volatile nature.
337
00:16:49,775 --> 00:16:53,177
They can explode in some of the
biggest bangs in the cosmos.
338
00:16:53,278 --> 00:16:56,280
[explosion blasts]
339
00:17:08,260 --> 00:17:12,063
ROWE: White dwarfs are the dead
remains of stars like the sun.
340
00:17:13,532 --> 00:17:16,067
Most of these zombie
stars slowly
341
00:17:16,168 --> 00:17:18,236
cooled down
over billions of years.
342
00:17:20,406 --> 00:17:22,106
Most, but not all.
343
00:17:25,744 --> 00:17:28,546
Some go out in a spectacular
explosion known
344
00:17:28,647 --> 00:17:30,314
as a type 1a supernova.
345
00:17:31,917 --> 00:17:33,351
A type 1a supernova
346
00:17:33,452 --> 00:17:35,753
is one of the most
violent, powerful,
347
00:17:35,854 --> 00:17:38,089
energetic events
in the universe.
348
00:17:38,190 --> 00:17:41,125
We are talking about
a star exploding.
349
00:17:41,226 --> 00:17:43,594
They can outshine
entire galaxies.
350
00:17:43,695 --> 00:17:45,663
They can create devastation over
351
00:17:45,764 --> 00:17:47,465
hundreds and hundreds of
light-years.
352
00:17:47,566 --> 00:17:49,000
They're a big deal.
353
00:17:51,670 --> 00:17:54,405
ROWE: We'd seen the aftermath
of these cosmic fireworks,
354
00:17:54,506 --> 00:17:57,542
but for over 60 years, we had
little direct evidence
355
00:17:57,643 --> 00:17:59,310
they came from white dwarfs.
356
00:18:01,613 --> 00:18:05,583
Then students from University
College London UK got lucky.
357
00:18:05,684 --> 00:18:09,587
While taking
routine photographs,
358
00:18:09,688 --> 00:18:11,889
they spotted
a supernova explosion
359
00:18:11,990 --> 00:18:14,792
in our own cosmic neighborhood.
360
00:18:14,893 --> 00:18:17,895
PLAIT: M82, the cigar galaxy,
is actually really
361
00:18:17,996 --> 00:18:19,964
close to us on cosmic terms.
362
00:18:20,065 --> 00:18:22,533
It's only about 12 million
light-years away.
363
00:18:22,634 --> 00:18:25,336
This makes it one of
the closest galaxies in the sky.
364
00:18:26,505 --> 00:18:29,273
The blast called
Supernova 2014J was
365
00:18:29,374 --> 00:18:33,244
the closest type 1a supernova
for over 20 years.
366
00:18:34,413 --> 00:18:36,247
Its proximity allowed us
to look for
367
00:18:36,348 --> 00:18:40,017
the signature of
a white dwarf supernova,
368
00:18:40,119 --> 00:18:42,019
a blast of gamma rays.
369
00:18:42,121 --> 00:18:47,125
Gamma rays are a type of light
that's incredibly energetic.
370
00:18:47,226 --> 00:18:49,760
They're the most energetic
type of rays,
371
00:18:49,862 --> 00:18:53,498
or photons, on
the electromagnetic spectrum.
372
00:18:53,599 --> 00:18:55,099
ROWE:
White dwarfs should release
373
00:18:55,200 --> 00:18:57,568
gamma rays when they explode.
374
00:18:57,669 --> 00:19:01,239
But dust in interstellar space
soaks up the rays,
375
00:19:01,340 --> 00:19:06,244
so unless an explosion is close
by, they're hard to detect.
376
00:19:06,345 --> 00:19:09,447
For years, astronomers had
been looking for the gamma rays
377
00:19:09,548 --> 00:19:12,116
that should be emitted by
a type 1a supernova,
378
00:19:12,217 --> 00:19:13,584
but no one had found them.
379
00:19:15,954 --> 00:19:18,022
ROWE: Now, scientists had
their chance
380
00:19:18,123 --> 00:19:20,758
and the technology to see
the elusive rays.
381
00:19:22,628 --> 00:19:24,795
Using ISA's integral satellite,
382
00:19:24,897 --> 00:19:26,931
they sifted through
the shockwaves sent out by
383
00:19:27,032 --> 00:19:29,500
the explosion in M82.
384
00:19:29,601 --> 00:19:32,537
It was tough, but finally,
they got a reading,
385
00:19:32,638 --> 00:19:35,306
the telltale signal of
gamma rays.
386
00:19:35,407 --> 00:19:38,276
It's the best evidence yet
for white dwarfs
387
00:19:38,377 --> 00:19:41,412
exploding in type 1a supernovas.
388
00:19:41,513 --> 00:19:46,484
The reason Supernova 2014J
was so cool is that this
389
00:19:46,585 --> 00:19:49,587
observation gave scientists
evidence, it's white dwarfs that
390
00:19:49,688 --> 00:19:53,124
explode to create this specific
type of supernova.
391
00:19:53,225 --> 00:19:55,660
ROWE:
So which white dwarfs fade out
392
00:19:55,761 --> 00:19:57,828
and which ones
go out with a bang?
393
00:20:00,799 --> 00:20:02,633
A survey of stars revealed
394
00:20:02,734 --> 00:20:07,271
around 30% of white dwarfs
live in binary systems,
395
00:20:07,372 --> 00:20:09,907
but white dwarfs are not
good neighbors.
396
00:20:10,008 --> 00:20:13,811
A white dwarf in a binary
system is... it's like a zombie.
397
00:20:13,912 --> 00:20:16,681
It's the corpse of a star
that used to be alive.
398
00:20:16,782 --> 00:20:18,716
But now it is eating
the material
399
00:20:18,817 --> 00:20:21,185
from a star that is still alive.
400
00:20:21,286 --> 00:20:23,854
They very literally suck
the material
401
00:20:23,956 --> 00:20:25,690
and suck the life
out of that star
402
00:20:25,791 --> 00:20:28,392
by swallowing up all of
its outer layers.
403
00:20:30,062 --> 00:20:32,697
ROWE: The white dwarf zombie
tendencies can backfire.
404
00:20:33,865 --> 00:20:36,834
Adding mass to
a white dwarf is like this.
405
00:20:36,935 --> 00:20:41,672
We keep adding mass from that
companion star
406
00:20:41,773 --> 00:20:45,343
a little bit of hydrogen
at a time,
407
00:20:45,444 --> 00:20:48,946
building up that atmosphere,
and for a long time,
408
00:20:49,047 --> 00:20:50,748
everything's fine.
409
00:20:50,849 --> 00:20:54,785
Until you add too much mass,
and you reach that critical
410
00:20:54,886 --> 00:20:57,054
threshold, and then...
411
00:21:00,459 --> 00:21:02,493
ROWE:
The real-world consequences of
412
00:21:02,594 --> 00:21:05,896
reaching the threshold
are devastating.
413
00:21:05,998 --> 00:21:09,600
The extra weight of gas stolen
from the companion star
414
00:21:09,701 --> 00:21:12,703
compresses carbon deep in
the core of the white dwarf.
415
00:21:14,473 --> 00:21:18,409
When the white dwarf reaches
1.4 times the mass of our sun,
416
00:21:18,510 --> 00:21:23,080
it hits a tipping point known
as the Chandrasekhar limit.
417
00:21:23,181 --> 00:21:25,616
You add up the mass little by
little by little until
418
00:21:25,717 --> 00:21:28,119
you get to that Chandrasekhar
limit and then blam,
419
00:21:28,220 --> 00:21:30,421
there's a supernova.
- ROWE: In a flash,
420
00:21:30,522 --> 00:21:32,990
carbon undergoes nuclear fusion,
421
00:21:33,091 --> 00:21:34,992
releasing a tremendous
amount of energy.
422
00:21:38,063 --> 00:21:39,563
FILIPPENKO:
If the white dwarf explodes
423
00:21:39,665 --> 00:21:41,132
at the Chandrasekhar limit,
424
00:21:41,233 --> 00:21:43,901
it's a little bit like
fireworks that all have
425
00:21:44,002 --> 00:21:45,670
the same amount of gunpowder.
426
00:21:45,771 --> 00:21:49,106
They'll all go off in the same
way, they'll be equally loud.
427
00:21:49,207 --> 00:21:51,275
Well, the supernovas
will be equally bright.
428
00:21:53,045 --> 00:21:55,279
ROWE: This equal brightness
of all type 1a
429
00:21:55,380 --> 00:21:58,549
supernovas is vital to
our understanding of space.
430
00:21:59,751 --> 00:22:03,321
Type 1a's are known as
standard candles
431
00:22:03,422 --> 00:22:05,923
and are useful tools for
calculating fast
432
00:22:06,024 --> 00:22:07,925
cosmic distances.
433
00:22:08,026 --> 00:22:10,161
They were the key
to the Nobel Prize winning
434
00:22:10,262 --> 00:22:12,897
discovery that the expansion
of our universe
435
00:22:12,998 --> 00:22:14,465
is accelerating.
436
00:22:14,566 --> 00:22:20,271
But what kind of companion star
triggers type 1a supernovas?
437
00:22:20,372 --> 00:22:25,176
For decades, the number one
suspect was red giant stars.
438
00:22:25,277 --> 00:22:26,410
HOPKINS: A red giant's
439
00:22:26,511 --> 00:22:30,314
a good candidate, because it's
a very big, puffy star.
440
00:22:30,415 --> 00:22:33,617
That material becomes easy
pickings for the white dwarf
441
00:22:33,719 --> 00:22:36,520
to siphon off until it gets
big enough to explode.
442
00:22:37,889 --> 00:22:40,024
ROWE: To prove the theory,
we needed to find
443
00:22:40,125 --> 00:22:43,961
evidence in the debris left
behind after a supernova.
444
00:22:44,062 --> 00:22:47,331
Stars are surprisingly
hardy objects.
445
00:22:47,432 --> 00:22:50,735
They can survive an explosion
of a nearby star.
446
00:22:50,836 --> 00:22:53,237
Some of these companion stars
should still be there.
447
00:22:53,338 --> 00:22:55,539
A lot of them will be, you know,
worse for the wear,
448
00:22:55,640 --> 00:22:57,742
but they'll still exist.
449
00:22:57,843 --> 00:22:59,677
ROWE: Scientists search
through the remains
450
00:22:59,778 --> 00:23:02,546
of 70 type 1a supernovas.
451
00:23:03,915 --> 00:23:05,850
Only one blast zone contained
452
00:23:05,951 --> 00:23:08,619
the glowing remains
of a red giant.
453
00:23:09,721 --> 00:23:12,923
The fact that we've only found
maybe this one example suggests
454
00:23:13,024 --> 00:23:15,192
that actually, they're not
quite the serial killers
455
00:23:15,293 --> 00:23:16,694
we thought.
456
00:23:16,795 --> 00:23:18,863
It's probably likely
that this is
457
00:23:18,964 --> 00:23:22,767
the minority of these types of
supernova explosions.
458
00:23:22,868 --> 00:23:26,303
Indeed, we now think that only
a small fraction of
459
00:23:26,405 --> 00:23:30,374
these white dwarf supernovas
involve a red giant,
460
00:23:30,475 --> 00:23:33,210
despite the fact that, in
the standard textbooks, for
461
00:23:33,311 --> 00:23:36,080
decades, that was
the preferred explanation.
462
00:23:37,382 --> 00:23:38,783
ROWE: If red giants don't cause
463
00:23:38,884 --> 00:23:41,619
the majority of
type 1a supernovas,
464
00:23:41,720 --> 00:23:43,487
what does?
465
00:23:43,588 --> 00:23:45,122
New evidence suggests
466
00:23:45,223 --> 00:23:47,024
colliding white dwarfs,
467
00:23:47,125 --> 00:23:49,326
star mergers that could exceed
468
00:23:49,428 --> 00:23:51,162
the Chandrasekhar limit,
469
00:23:51,263 --> 00:23:54,365
producing explosions with
different brightness.
470
00:23:54,466 --> 00:23:57,168
But if the explosions
vary in brightness,
471
00:23:57,269 --> 00:23:58,969
can they still be used
472
00:23:59,070 --> 00:24:01,205
as standard candles?
473
00:24:01,306 --> 00:24:04,475
PONTZEN: If we don't really know
what a type 1a supernova is,
474
00:24:04,576 --> 00:24:05,976
then when we use them to map out
475
00:24:06,077 --> 00:24:08,979
the universe and the way
the universe is expanding,
476
00:24:09,080 --> 00:24:12,450
we just can't be sure any longer
what it is we're looking at.
477
00:24:12,551 --> 00:24:14,084
If we're wrong about that,
478
00:24:14,186 --> 00:24:16,887
then we're wrong about so many
other things that our whole
479
00:24:16,988 --> 00:24:18,456
model of the universe
falls apart.
480
00:24:19,524 --> 00:24:22,626
ROWE: Is our understanding of
the cosmos completely wrong?
481
00:24:35,974 --> 00:24:39,944
ROWE: White dwarfs explode in
spectacular type 1a supernovas.
482
00:24:41,480 --> 00:24:44,215
They're a crucial tool for
measuring the universe,
483
00:24:44,316 --> 00:24:46,150
but there is a problem.
484
00:24:48,086 --> 00:24:50,321
The standard model
says that white dwarfs
485
00:24:50,422 --> 00:24:54,258
gradually steal mass
from a red giant star
486
00:24:54,359 --> 00:24:56,160
until they reach a tipping point
487
00:24:56,261 --> 00:24:57,895
called the Chandrasekhar limit.
488
00:25:00,632 --> 00:25:03,601
But recent observations
proved this doesn't explain
489
00:25:03,702 --> 00:25:06,337
how most type 1a
supernovas occur.
490
00:25:07,906 --> 00:25:12,009
The majority of type 1a
explosions remain a mystery.
491
00:25:12,110 --> 00:25:14,678
We call the explosions from
white dwarfs standard candles,
492
00:25:14,779 --> 00:25:16,013
but they're really not
that standard.
493
00:25:16,114 --> 00:25:18,582
We actually think there's
different types of explosions.
494
00:25:18,683 --> 00:25:21,218
THALLER: It may be imperative
to our understanding
495
00:25:21,319 --> 00:25:23,153
of the entire universe
that we really get
496
00:25:23,255 --> 00:25:25,689
this straight, because
the reason we think
497
00:25:25,790 --> 00:25:27,958
the expansion rate of
the universe is accelerating
498
00:25:28,059 --> 00:25:30,394
is based on the brightness of
type 1 supernovas
499
00:25:30,495 --> 00:25:33,898
all being the same,
and maybe that's not the case.
500
00:25:33,999 --> 00:25:36,667
ROWE: Researchers suspected
a theoretical type of
501
00:25:36,768 --> 00:25:38,502
merger could be responsible
502
00:25:38,603 --> 00:25:42,006
for more type 1a supernovas,
503
00:25:42,073 --> 00:25:45,776
the result of two white dwarfs
crashing together.
504
00:25:45,877 --> 00:25:48,779
But this messes with the math.
505
00:25:48,880 --> 00:25:51,916
The Chandrasekhar limit says
white dwarfs should
506
00:25:52,017 --> 00:25:53,150
explode when they reach
507
00:25:53,251 --> 00:25:56,687
1.4 times the mass of our sun.
508
00:25:56,788 --> 00:26:00,024
Two white dwarfs colliding
can exceed this mass,
509
00:26:00,125 --> 00:26:02,526
and more mass means
a bigger bang
510
00:26:02,594 --> 00:26:05,129
and a brighter explosion.
511
00:26:07,432 --> 00:26:08,332
You're not adding gas
512
00:26:08,433 --> 00:26:10,034
little by little,
you're adding a whole
513
00:26:10,135 --> 00:26:12,369
other white dwarf...
That will go off.
514
00:26:12,470 --> 00:26:14,138
It will look like
a type 1 supernova,
515
00:26:14,239 --> 00:26:15,673
but it won't be
the standard candle.
516
00:26:15,774 --> 00:26:17,308
It'll be brighter than
we expect.
517
00:26:17,409 --> 00:26:22,446
ROWE: But no white dwarf mergers
have been found, because
518
00:26:22,547 --> 00:26:26,617
detecting one after it happens
is virtually impossible.
519
00:26:26,718 --> 00:26:28,819
HOPKINS: If two white dwarfs
merge together,
520
00:26:28,920 --> 00:26:32,356
it's almost impossible to tell,
because the DNA of the two
521
00:26:32,457 --> 00:26:35,259
systems is all mixed together,
and it's all identical.
522
00:26:35,327 --> 00:26:38,395
You can't tell that there was
a separate companion in
523
00:26:38,496 --> 00:26:39,697
the first place.
524
00:26:39,798 --> 00:26:42,600
SUTTER: So we can't just look at
when there's a bright flash.
525
00:26:42,701 --> 00:26:44,935
We have to go look for
the ticking time bombs in
526
00:26:45,036 --> 00:26:46,570
the galaxy.
527
00:26:46,671 --> 00:26:50,140
ROWE: Astronomers
investigating a strange shaped
528
00:26:50,241 --> 00:26:52,876
cloud of gas made
a breakthrough.
529
00:26:52,978 --> 00:26:56,814
Using ESO's Very
Large Telescope,
530
00:26:56,915 --> 00:27:02,252
they focused in on a planetary
nebula called Henize 2-428.
531
00:27:02,354 --> 00:27:05,522
Planetary nebulas are
normally symmetric,
532
00:27:05,624 --> 00:27:07,191
because red giants shed
533
00:27:07,292 --> 00:27:11,328
their outer layers evenly
as they become white dwarfs.
534
00:27:11,429 --> 00:27:14,198
But this one is lopsided.
535
00:27:14,299 --> 00:27:16,934
We think, in this case, there
might be the presence of
536
00:27:17,035 --> 00:27:21,538
a companion star that shapes
and twists and sculpts
537
00:27:21,640 --> 00:27:23,540
that planetary nebula.
538
00:27:25,610 --> 00:27:26,844
ROWE: Researchers peeled back
539
00:27:26,945 --> 00:27:30,614
the gaseous layers and
discovered something shocking,
540
00:27:30,715 --> 00:27:33,717
a two-star system made up of
541
00:27:33,818 --> 00:27:36,420
the most massive orbiting
white dwarf pair
542
00:27:36,521 --> 00:27:37,621
ever discovered.
543
00:27:39,591 --> 00:27:43,527
Each star is 90%
as massive as our sun,
544
00:27:43,628 --> 00:27:45,295
and they're so close together,
they take
545
00:27:45,397 --> 00:27:47,331
just four hours
to orbit each other.
546
00:27:47,432 --> 00:27:50,668
And they're getting closer.
547
00:27:50,769 --> 00:27:54,838
SUTTER: If you've ever seen
a car crash about to happen,
548
00:27:54,939 --> 00:27:58,175
you know that sense of
inevitability
549
00:27:58,276 --> 00:27:59,677
as you witness that.
550
00:27:59,778 --> 00:28:01,745
That's what we're seeing in
this system.
551
00:28:01,846 --> 00:28:06,083
We see these two massive white
dwarfs spiraling closer
552
00:28:06,184 --> 00:28:10,954
and closer and closer, and we
know that disaster is coming.
553
00:28:11,056 --> 00:28:12,990
ROWE:
In around 700 million years,
554
00:28:13,091 --> 00:28:15,392
these stars will
merge and explode
555
00:28:15,493 --> 00:28:17,661
in a type 1a supernova.
556
00:28:22,200 --> 00:28:24,768
Now, thanks to the discovery
of more systems
557
00:28:24,869 --> 00:28:26,637
like Henize 2-428,
558
00:28:26,738 --> 00:28:29,406
we think white dwarf
collisions could be responsible
559
00:28:29,507 --> 00:28:32,176
for the majority of
type 1a supernovas.
560
00:28:32,277 --> 00:28:34,511
[explosion blasts]
561
00:28:34,612 --> 00:28:38,182
Two white dwarfs
can merge together.
562
00:28:38,283 --> 00:28:40,584
And if the sum of their masses
is greater than
563
00:28:40,685 --> 00:28:42,152
1.4 solar masses,
564
00:28:42,287 --> 00:28:44,288
then you can get
a Super-Chandra type 1a.
565
00:28:44,389 --> 00:28:46,824
ROWE: We've now observed
566
00:28:46,925 --> 00:28:48,859
nine Super-Chandra explosions,
567
00:28:50,495 --> 00:28:52,196
and to complicate
matters further,
568
00:28:52,297 --> 00:28:55,966
we've spotted another form of
white dwarf supernovas,
569
00:28:56,067 --> 00:28:58,001
Sub-Chandra type 1as.
570
00:28:59,871 --> 00:29:03,173
These mysterious white dwarfs
that we don't quite understand
571
00:29:03,274 --> 00:29:06,677
die off much quicker than
regular white dwarf supernovas.
572
00:29:06,811 --> 00:29:08,445
[explosion blasts]
573
00:29:08,546 --> 00:29:10,814
ROWE: The explosions are less
violent than normal
574
00:29:10,915 --> 00:29:14,017
type 1a supernovas
and fade away faster.
575
00:29:14,119 --> 00:29:16,386
But we don't know why.
576
00:29:18,256 --> 00:29:19,957
Maybe it has something to
do with
577
00:29:20,058 --> 00:29:22,292
the properties of the star
or the rotation,
578
00:29:22,393 --> 00:29:24,595
but the Chandrasekhar limit
may not be so exact.
579
00:29:24,696 --> 00:29:27,197
It's kind of
a Chandrasekhar range.
580
00:29:27,298 --> 00:29:30,134
The physics textbooks are
now being sort of rewritten,
581
00:29:30,235 --> 00:29:34,538
or at least modified, because
we know that not all type 1a
582
00:29:34,639 --> 00:29:38,008
supernovas come from Chandra
mass white dwarfs.
583
00:29:38,109 --> 00:29:41,979
There's actually a variety of
type 1a supernovas,
584
00:29:42,080 --> 00:29:46,350
a variety of white dwarf masses
and configurations
585
00:29:46,451 --> 00:29:47,618
that can explode.
586
00:29:49,120 --> 00:29:52,189
ROWE: These new discoveries
mean researchers now study
587
00:29:52,290 --> 00:29:55,359
the chemistry and duration of
type 1a supernovas,
588
00:29:55,460 --> 00:29:57,327
not just their brightness.
589
00:30:01,099 --> 00:30:05,068
The deeper we investigate,
the more mysteries we uncover,
590
00:30:05,170 --> 00:30:08,772
like rogue white dwarfs
streaking across the galaxy
591
00:30:08,873 --> 00:30:13,977
and tiny stars that explode
over and over again.
592
00:30:14,078 --> 00:30:16,479
Can these odd white dwarfs
shed more
593
00:30:16,548 --> 00:30:19,616
light on the mystery of type
1a supernovas?
594
00:30:30,562 --> 00:30:31,461
ROWE: White dwarfs are
595
00:30:31,563 --> 00:30:33,797
surprisingly difficult
to understand.
596
00:30:35,600 --> 00:30:38,468
They behave in completely
unexpected ways.
597
00:30:40,238 --> 00:30:43,173
But these oddballs may
help answer
598
00:30:43,241 --> 00:30:46,844
the remaining questions about
type 1a supernovas.
599
00:30:46,945 --> 00:30:49,213
These are white dwarfs,
but not as we know them.
600
00:30:50,448 --> 00:30:55,385
ROWE: 2017... astronomers spot
a rebellious star
601
00:30:55,486 --> 00:30:57,855
raising hell in
the Little Dipper constellation.
602
00:30:59,624 --> 00:31:02,459
It's like a zombie, but this
isn't one shambling down
603
00:31:02,560 --> 00:31:04,828
the road,
it runs like Usain Bolt.
604
00:31:04,929 --> 00:31:07,598
This thing is screaming
through the galaxy at a much
605
00:31:07,699 --> 00:31:10,000
higher speed than you'd expect
for a star like it.
606
00:31:12,070 --> 00:31:15,138
ROWE: The white dwarf
called LP 40-365
607
00:31:15,240 --> 00:31:16,974
is moving incredibly fast
608
00:31:17,075 --> 00:31:18,675
towards the edge
of the Milky Way.
609
00:31:18,776 --> 00:31:24,281
It's not the only star
behaving oddly... in 2019,
610
00:31:24,382 --> 00:31:27,384
we spotted three more
white dwarfs racing across
611
00:31:27,485 --> 00:31:28,852
the galaxy.
612
00:31:28,953 --> 00:31:30,854
Finding one white dwarf
blasting its way
613
00:31:30,955 --> 00:31:32,656
through space is weird enough.
614
00:31:32,757 --> 00:31:35,692
But to find three more, that's
telling you that something is
615
00:31:35,793 --> 00:31:37,194
going on, and whatever it is
616
00:31:37,295 --> 00:31:40,063
that's going on happens a lot.
617
00:31:40,164 --> 00:31:41,832
ROWE:
So what sent these renegades
618
00:31:41,933 --> 00:31:44,101
racing across the galaxy?
619
00:31:44,202 --> 00:31:47,971
LP 40-365 and these other
weird white dwarfs
620
00:31:48,072 --> 00:31:51,074
could be the results
of failed supernovas.
621
00:31:51,175 --> 00:31:52,910
People have theorized that maybe
622
00:31:53,011 --> 00:31:54,978
these things didn't
finish exploding.
623
00:31:55,079 --> 00:31:56,313
And if so, we should find
624
00:31:56,414 --> 00:31:59,449
some unburnt fractions
wandering around the galaxy.
625
00:32:01,052 --> 00:32:04,621
ROWE: In the last 20 years,
we've spotted some unusually dim
626
00:32:04,722 --> 00:32:07,057
supernovas that could have sent
627
00:32:07,158 --> 00:32:11,194
LP 40-365 and friends flying.
628
00:32:11,296 --> 00:32:14,932
So what looks like happened is
that in a binary pair,
629
00:32:15,033 --> 00:32:16,934
there was stuff dumping
onto a white dwarf,
630
00:32:17,035 --> 00:32:19,569
and we were about to have
a type 1 supernova.
631
00:32:19,671 --> 00:32:22,606
But the type 1 supernova
didn't go off symmetrically.
632
00:32:22,707 --> 00:32:25,876
Some of it actually exploded,
and some of it didn't.
633
00:32:25,977 --> 00:32:29,246
That energy didn't go out in
all directions.
634
00:32:29,347 --> 00:32:31,949
And one of the things that
occurred is that these stars
635
00:32:32,050 --> 00:32:35,252
got sent hurling across space
at these incredible speeds.
636
00:32:39,190 --> 00:32:42,059
ROWE: We call them
type 1ax supernovas.
637
00:32:42,160 --> 00:32:45,696
They could make up between
10 and 30%
638
00:32:45,797 --> 00:32:48,265
of type 1a supernovas.
639
00:32:48,366 --> 00:32:50,867
Many could throw out
a runaway star.
640
00:32:52,437 --> 00:32:55,839
But we still don't know why
the supernova fails.
641
00:32:55,940 --> 00:32:58,976
PLAIT: A funny thing
about science is things
642
00:32:59,077 --> 00:33:02,112
that fail still teach you
what's going on.
643
00:33:02,213 --> 00:33:04,548
Why are these ones different?
Were they not massive enough?
644
00:33:04,649 --> 00:33:06,683
Where they too massive?
Was the companion star
645
00:33:06,784 --> 00:33:08,885
not feeding them the material
the right way?
646
00:33:08,987 --> 00:33:11,655
Something happened there to
make these stars
647
00:33:11,756 --> 00:33:14,925
not basically blow
themselves to bits.
648
00:33:15,026 --> 00:33:17,060
And that's telling us
something about
649
00:33:17,161 --> 00:33:19,830
the way type 1as do explode.
650
00:33:21,499 --> 00:33:23,800
ROWE: It seems that life
in a binary star system
651
00:33:23,901 --> 00:33:25,902
can be rough for white dwarfs,
652
00:33:26,004 --> 00:33:29,239
but for some lucky stars,
their lives can
653
00:33:29,340 --> 00:33:31,174
be more mellow.
654
00:33:31,275 --> 00:33:33,377
Just because a white dwarf
655
00:33:33,478 --> 00:33:35,278
has a normal star companion that
656
00:33:35,380 --> 00:33:38,815
it's stealing material from
does not spell a death sentence
657
00:33:38,916 --> 00:33:40,217
for that white dwarf.
658
00:33:40,318 --> 00:33:43,253
ROWE: February 2013.
659
00:33:43,354 --> 00:33:46,757
Astronomers discover a star in
the Andromeda galaxy
660
00:33:46,858 --> 00:33:50,961
that flashes over and over
and over again.
661
00:33:51,062 --> 00:33:52,129
With each flare,
662
00:33:52,230 --> 00:33:55,932
it shines a million times
brighter than our sun
663
00:33:56,034 --> 00:33:58,268
before dimming to its
normal state.
664
00:33:58,369 --> 00:34:03,340
It's called M31N 2018-12a.
665
00:34:06,110 --> 00:34:09,413
This is not a supernova,
it's its little sibling,
666
00:34:09,514 --> 00:34:10,914
a nova.
667
00:34:11,015 --> 00:34:13,583
But what's weird about this
one is that it happens
668
00:34:13,684 --> 00:34:14,851
every year.
669
00:34:14,952 --> 00:34:18,488
Astronomers have known for
a long time that there are these
670
00:34:18,589 --> 00:34:21,358
cases of these nova that go off,
671
00:34:21,459 --> 00:34:23,360
you know, somewhat regularly,
every 10 years,
672
00:34:23,461 --> 00:34:24,661
every 100 years.
673
00:34:24,762 --> 00:34:26,396
But finding one that goes off
674
00:34:26,497 --> 00:34:29,032
every year is
a remarkable discovery.
675
00:34:30,568 --> 00:34:31,968
ROWE: Much like supernovas,
676
00:34:32,070 --> 00:34:34,237
novas occur in a close
binary system,
677
00:34:34,338 --> 00:34:37,274
where a white dwarf and
another star orbit each other.
678
00:34:39,944 --> 00:34:41,812
The white dwarf pulls in
hydrogen
679
00:34:41,913 --> 00:34:43,680
from the companion star.
680
00:34:43,781 --> 00:34:46,149
The gas falls onto its surface.
681
00:34:46,250 --> 00:34:48,718
And so as
that hydrogen piles up,
682
00:34:48,820 --> 00:34:50,921
eventually, it gets to
the point where
683
00:34:51,022 --> 00:34:54,191
it can fuse into helium
and goes bang.
684
00:34:55,960 --> 00:34:56,860
ROWE: In supernovas,
685
00:34:56,961 --> 00:35:00,163
fusion happens deep inside
the star's core,
686
00:35:01,532 --> 00:35:05,335
but in novas, fusion only
occurs on the surface.
687
00:35:05,403 --> 00:35:09,406
An explosion flares across
the white dwarf's exterior,
688
00:35:09,507 --> 00:35:13,510
hurling unburned hydrogen
out into space.
689
00:35:13,611 --> 00:35:17,647
The result... an object
called a remnant.
690
00:35:17,715 --> 00:35:23,386
The remnant from Nova M31N
is 400 light-years wide.
691
00:35:23,488 --> 00:35:25,122
This particular remnant is much
692
00:35:25,223 --> 00:35:27,891
bigger than even
supernova remnants.
693
00:35:27,992 --> 00:35:29,526
It's much larger, much denser
694
00:35:29,627 --> 00:35:31,461
and brighter than most
normal remnants are.
695
00:35:31,562 --> 00:35:32,562
But that makes sense
696
00:35:32,663 --> 00:35:34,798
if the star flares up so often.
697
00:35:34,899 --> 00:35:38,368
Think about the star flaring
away for millions of years.
698
00:35:38,469 --> 00:35:42,572
You build up a gigantic
nova remnant.
699
00:35:42,673 --> 00:35:44,107
ROWE:
The repeating flares explain
700
00:35:44,208 --> 00:35:45,575
the huge size of the remnant.
701
00:35:45,676 --> 00:35:48,945
But why does the nova explode
so frequently?
702
00:35:49,046 --> 00:35:53,183
Classically, we thought that
when a nova went off
703
00:35:53,284 --> 00:35:54,384
on the surface of
704
00:35:54,485 --> 00:35:58,221
a white dwarf star that
the white dwarf star's mass
705
00:35:58,322 --> 00:35:59,489
didn't change very much.
706
00:35:59,590 --> 00:36:01,291
Or maybe it got
a little smaller.
707
00:36:01,392 --> 00:36:04,661
Now we think that after a nova,
708
00:36:04,762 --> 00:36:07,430
the white dwarf
gains a bit of mass.
709
00:36:09,033 --> 00:36:12,736
ROWE: Recurrent novas, like
M31N, steal more mass from
710
00:36:12,837 --> 00:36:15,906
their companion star than they
blow off in each explosion.
711
00:36:17,108 --> 00:36:18,875
Some gain more and more mass,
712
00:36:18,976 --> 00:36:21,845
exploding more frequently
until they reach
713
00:36:21,946 --> 00:36:23,980
the Chandrasekhar limit
714
00:36:24,081 --> 00:36:26,983
and go full-on supernova.
715
00:36:27,084 --> 00:36:29,486
M31N may very well be
716
00:36:29,587 --> 00:36:32,088
the missing link that shows us
717
00:36:32,190 --> 00:36:35,258
that some nova systems
eventually become
718
00:36:35,359 --> 00:36:36,626
supernova systems.
719
00:36:36,727 --> 00:36:38,995
ROWE:
Working out how novas become
720
00:36:39,096 --> 00:36:42,065
supernovas and why some
supernovas fail
721
00:36:43,968 --> 00:36:47,671
might help us understand what
makes white dwarfs explode.
722
00:36:50,474 --> 00:36:52,742
But just when we think
we get a break,
723
00:36:52,843 --> 00:36:55,078
white dwarfs hit us
with another bombshell...
724
00:36:55,179 --> 00:36:57,380
death rays.
725
00:37:09,727 --> 00:37:12,796
ROWE: White dwarfs can explode
in violent supernovas,
726
00:37:15,733 --> 00:37:18,501
but that's not
their only deadly trick.
727
00:37:18,603 --> 00:37:20,737
They might also create the most
728
00:37:20,838 --> 00:37:24,774
magnetic and terrifying beast
in the universe...
729
00:37:24,875 --> 00:37:27,143
A magnetar.
730
00:37:27,245 --> 00:37:30,347
Magentars are scary.
They just are.
731
00:37:30,448 --> 00:37:31,481
I mean, it's even in the name.
732
00:37:31,582 --> 00:37:33,883
The word magnetar sounds scary.
733
00:37:33,985 --> 00:37:35,452
They're the reigning champion of
734
00:37:35,553 --> 00:37:37,687
the largest magnetic field in
the universe.
735
00:37:40,191 --> 00:37:44,828
SUTTER: The magnetic fields
around magnetars are so strong
736
00:37:44,929 --> 00:37:48,965
that they can stretch
and distort individual atoms.
737
00:37:49,066 --> 00:37:52,836
They can turn an atom into
a long, thin pencil shape.
738
00:37:52,937 --> 00:37:56,339
Once you start stretching
atoms out into this shape,
739
00:37:56,440 --> 00:37:59,676
they can't bond together
in the usual ways anymore.
740
00:37:59,777 --> 00:38:01,411
And so you can just throw out
741
00:38:01,512 --> 00:38:04,514
every chemistry textbook
in the world.
742
00:38:04,615 --> 00:38:06,850
BULLOCK: If an astronaut were
unlucky enough to get close to
743
00:38:06,951 --> 00:38:08,318
a magnetar, say, within
744
00:38:08,419 --> 00:38:11,888
600, 700 miles,
the whole body of the astronaut
745
00:38:11,989 --> 00:38:13,256
would be completely obliterated.
746
00:38:13,357 --> 00:38:15,625
They would more
or less dissolve.
747
00:38:15,726 --> 00:38:18,495
ROWE: The origin of these
fearsome creatures is a mystery,
748
00:38:18,596 --> 00:38:21,364
but it must be something
very violent.
749
00:38:21,465 --> 00:38:24,567
We think they send out
a clue as they form,
750
00:38:24,669 --> 00:38:28,738
powerful blasts of energy
shooting across the cosmos.
751
00:38:28,839 --> 00:38:32,742
In the past few decades,
we've noticed these very odd,
752
00:38:32,843 --> 00:38:35,211
very confusing and very brief
753
00:38:35,313 --> 00:38:39,549
flashes of intense radio energy.
754
00:38:39,650 --> 00:38:42,919
ROWE: They're known as fast
radio bursts, or FRBs.
755
00:38:44,088 --> 00:38:46,990
Some FRBs don't repeat.
They're one and done.
756
00:38:47,091 --> 00:38:48,892
So you're talking about
an incredible amount
757
00:38:48,993 --> 00:38:51,428
of energy released in less
than a second,
758
00:38:51,529 --> 00:38:52,862
then it's over.
759
00:38:52,963 --> 00:38:55,231
ROWE: Because these
non-repeating FRBs are
760
00:38:55,333 --> 00:38:59,469
so powerful, we think they could
come from a huge collision.
761
00:38:59,570 --> 00:39:02,238
The heavier and denser
the objects colliding,
762
00:39:03,908 --> 00:39:05,008
the bigger the bang.
763
00:39:06,410 --> 00:39:10,447
New research suggests a white
dwarf star hitting a dense,
764
00:39:10,548 --> 00:39:13,917
heavy neutron star could be
enough to birth
765
00:39:14,018 --> 00:39:15,985
a magnetar,
766
00:39:16,087 --> 00:39:19,089
sending out FRBs in the process.
767
00:39:19,190 --> 00:39:22,592
A neutron star is
like a white dwarf.
768
00:39:22,693 --> 00:39:26,096
Even more so...
It is the leftover core
769
00:39:26,197 --> 00:39:28,365
of a giant star.
770
00:39:28,466 --> 00:39:31,134
They're effectively giant
balls of neutrons
771
00:39:31,235 --> 00:39:32,168
squeezed together
772
00:39:32,269 --> 00:39:34,771
into things about the size
of a city.
773
00:39:34,872 --> 00:39:37,774
SUTTER: You have a neutron star,
an incredibly nasty,
774
00:39:37,875 --> 00:39:40,844
complicated exotic object
and a white dwarf,
775
00:39:40,945 --> 00:39:43,546
an incredibly nasty,
ugly, complicated object,
776
00:39:43,647 --> 00:39:45,882
crashing headlong into
each other.
777
00:39:47,585 --> 00:39:49,719
ROWE: As the two stars
orbit more closely,
778
00:39:49,820 --> 00:39:52,489
the neutron star strips gas
from the white dwarf.
779
00:39:53,958 --> 00:39:57,727
This material spirals
onto the neutron star,
780
00:39:57,795 --> 00:40:00,196
causing it to spin faster
and faster.
781
00:40:02,633 --> 00:40:06,069
The rapid rotation amplifies
its magnetic fields
782
00:40:07,438 --> 00:40:10,640
until the two stars collide,
783
00:40:10,741 --> 00:40:13,743
creating
a very magnetic monster,
784
00:40:13,844 --> 00:40:15,745
a magnetar.
785
00:40:15,846 --> 00:40:17,680
It's a turbulent situation.
786
00:40:17,782 --> 00:40:19,783
You could think of it as
a newborn baby coming into
787
00:40:19,884 --> 00:40:22,085
the world,
kicking and screaming.
788
00:40:22,186 --> 00:40:23,553
ROWE: The turbulence produces
789
00:40:23,654 --> 00:40:26,456
a powerful blast of
electromagnetic radiation.
790
00:40:28,859 --> 00:40:32,929
It races out of the collision
site at the speed of light
791
00:40:33,030 --> 00:40:36,800
until we detect it
as a fast radio burst.
792
00:40:38,502 --> 00:40:41,571
We can hear the screams of
agony from millions
793
00:40:41,672 --> 00:40:42,772
of light-years away,
794
00:40:42,873 --> 00:40:46,910
and those screams are
the fast radio bursts.
795
00:40:47,011 --> 00:40:48,912
This could be the most
difficult childbirth in
796
00:40:49,013 --> 00:40:49,979
the cosmos.
797
00:40:55,286 --> 00:40:58,121
ROWE: Few suspected
that white dwarfs could create
798
00:40:58,222 --> 00:41:00,590
something as violent as
a magnetar.
799
00:41:03,561 --> 00:41:06,029
White dwarfs are emerging
from out of
800
00:41:06,130 --> 00:41:08,965
the shadows and taking
their rightful place
801
00:41:09,066 --> 00:41:11,801
as one of the most
fascinating objects
802
00:41:11,902 --> 00:41:13,536
in the universe.
803
00:41:13,637 --> 00:41:16,206
When we first observed white
dwarfs, they were weird.
804
00:41:16,307 --> 00:41:19,342
They were curious,
but just like a sideshow.
805
00:41:19,443 --> 00:41:21,544
But now white dwarfs
are showing us
806
00:41:21,645 --> 00:41:23,546
what they're truly capable of.
807
00:41:23,614 --> 00:41:25,348
STRAUGHN: White dwarfs
can sort of be seen
808
00:41:25,449 --> 00:41:27,217
as these underdogs
of the universe,
809
00:41:27,318 --> 00:41:30,353
but it's really become
an exciting and cutting edge
810
00:41:30,454 --> 00:41:32,822
area of research.
811
00:41:32,923 --> 00:41:34,290
THALLER: Now we think
these objects may have
812
00:41:34,391 --> 00:41:36,993
a lot of exciting science
to deliver, things like,
813
00:41:37,094 --> 00:41:38,728
will the universe
expand forever?
814
00:41:38,829 --> 00:41:40,563
What is the ultimate fate of
the universe?
815
00:41:40,664 --> 00:41:44,801
All of that may be waiting for
us inside a white dwarf.
816
00:41:44,902 --> 00:41:47,504
PLAIT: Discount these things
at your own risk,
817
00:41:47,605 --> 00:41:48,805
because honestly,
818
00:41:48,906 --> 00:41:51,241
they are one of the driving
forces in the universe.
819
00:41:51,342 --> 00:41:54,310
Just because it's little
don't mean it ain't bad.
820
00:41:54,411 --> 00:41:56,246
Don't underestimate
a white dwarf.
65772
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