## Tale of a Doomed Galaxy

### Part 1

About 3 billion years ago, if there was intelligent life on the galaxy we call PG 1302-102, it should have known it was in serious trouble.

Our galaxy has a supermassive black hole in the middle. But that galaxy had two. One was about ten times as big as the other. Taken together, they weighed a billion times as much as our Sun.

They gradually spiraled in towards each other… and then, suddenly, one fine morning, they collided. The resulting explosion was 10 million times more powerful than a supernova—more powerful than anything astronomers here on Earth have ever seen! It was probably enough to wipe out all life in that galaxy.

We haven’t actually seen this yet. The light and gravitational waves from the disaster are still speeding towards us. They should reach us in roughly 100,000 years. We’re not sure when.

Right now, we see the smaller black hole still orbiting the big one, once every 5 years. In fact it’s orbiting once every 4 years! But thanks to the expansion of the universe, PG 1302-102 is moving away from us so fast that time on that distant galaxy looks significantly slowed down to us.

Orbiting once every 4 years: that doesn’t sound so fast. But the smaller black hole is about 2000 times more distant from its more massive companion than Pluto is from our Sun! So in fact it’s moving at very high speed – about 1% of the speed of light. We can actually see it getting redshifted and then blueshifted as it zips around. And it will continue to speed up as it spirals in.

What exactly will happen when these black holes collide? It’s too bad we won’t live to see it. We’re far enough that it will be perfectly safe to watch from here! But the human race knows enough about physics to say quite a lot about what it will be like. And we’ve built some amazing machines to detect the gravitational waves created by collisions like this—so as time goes on, we’ll know even more.

### Part 2

Even before the black holes at the heart of PG 1302-102 collided, life in that galaxy would have had a quasar to contend with!

This is a picture of Centaurus A, a much closer galaxy with a quasar in it. A quasar is huge black hole in the middle of a galaxy—a black hole that’s eating lots of stars, which rip apart and form a disk of hot gas as they spiral in. ‘Hot’ is an understatement, since this gas moves near the speed of light. It gets so hot that it pumps out intense jets of particles – from its north and south poles. Some of these particles even make it to Earth.

Any solar system in Centaurus A that gets in the way of those jets is toast.

And these jets create lots of radiation, from radio waves to X-rays. That’s how we can see quasars from billions of light years away. Quasars are the brightest objects in the universe, except for short-lived catastrophic events like the black hole collisions and gamma-ray bursts from huge dying stars.

It’s hard to grasp the size and power of such things, but let’s try. You can’t see the black hole in the middle of this picture, but it weighs 55 million times as much as our Sun. The blue glow of the jets in this picture is actually X rays. The jet at upper left is 13,000 light years long, made of particles moving at half the speed of light.

A typical quasar puts out a power of roughly 1040 watts. They vary a lot, but let’s pick this number as our ‘standard quasar’.

But what does 1040 watts actually mean? For comparison, the Sun puts out 4 x 1026 watts. So, we’re talking 30 trillion Suns. But even that’s too big a number to comprehend!

Maybe it would help to say that the whole Milky Way puts out 5 x 1036 watts. So a single quasar, at the center of one galaxy, can have the power of 2000 galaxies like ours.

Or, we can work out how much energy would be produced if the entire mass of the Moon were converted into energy. I’m getting 6 x 1039 joules. That’s a lot! But our standard quasar is putting out a bit more power than if it were converting one Moon into energy each second.

But you can’t just turn matter completely into energy: you need an equal amount of antimatter, and there’s not that much around. A quasar gets its power the old-fashioned way: by letting things fall down. In this case, fall down into a black hole.

To power our standard quasar, 10 stars need to fall into the black hole every year. The biggest quasars eat 1000 stars a year. The black hole in our galaxy gets very little to eat, so we don’t have a quasar.

There are short-lived events much more powerful than a quasar. For example, a gamma-ray burst, formed as a hypergiant star collapses into a black hole. A powerful gamma-ray burst can put out 10^44 watts for a few seconds. That’s equal to 10,000 quasars! But quasars last a long, long time.

So this was life in PG 1302-102 before things got really intense – before its two black holes spiraled into each other and collided. What was that collision like? I’ll talk about that next time.

The above picture of Centaurus A was actually made from images taken by three separate telescopes. The orange glow is submillimeter radiation – between infrared and microwaves—detected by the Atacama Pathfinder Experiment (APEX) telescope in Chile. The blue glow is X-rays seen by the Chandra X-ray Observatory. The rest is a photo taken in visible light by the Wide Field Imager on the Max-Planck/ESO 2.2 meter telescope, also located in Chile. This shows the dust lanes in the galaxy and background stars.

### Part 3

What happened at the instant the supermassive black holes in the galaxy PG 1302-102 finally collided?

We’re not sure yet, because the light and gravitational waves will take time to get here. But physicists are using computers to figure out what happens when black hole collide!

Here you see some results. The red blobs are the event horizons of two black holes.

First the black holes orbit each other, closer and closer, as they lose energy by emitting gravitational radiation. This is called the ‘inspiral’ phase.

Then comes the ‘plunge’ and ‘merger’. They plunge towards each other. A thin bridge forms between them, which you see here. Then they completely merge.

Finally you get a single black hole, which oscillates and then calms down. This is called the ‘ringdown’, because it’s like a bell ringing, loudly at first and then more quietly. But instead of emitting sound, it’s emitting gravitational waves—ripples in the shape of space!

In the top picture, the black holes have the same mass: one looks smaller, but that’s because it’s farther away. In the bottom picture, the black hole at left is twice as massive.

Here’s one cool discovery. An earlier paper had argued there could be two bridges, except in very symmetrical situations. If that were true, a black hole could have the topology of a torus for a little while. But these calculations showed that – at least in the cases they looked at—there’s just one bridge.

So, you can’t have black hole doughnuts. At least not yet.

These calculations were done using free software called SpEC. But before you try to run it at home: the team that puts out this software says:

Because of the steep learning curve and complexity of SpEC, new users are typically introduced to SpEC through a collaboration with experienced SpEC users.

It probably requires a lot of computer power, too. These calculations are very hard. We know the equations; they’re just tough to solve. The first complete simulation of an inspiral, merger and ringdown was done in 2005.

The reason people want to simulate colliding black holes is not mainly to create pretty pictures, or even understand what happens to the event horizon. It’s to understand the gravitational waves they will produce! People are building better and better gravitational wave detectors—more on that later—but we still haven’t seen gravitational waves. This is not surprising: they’re very weak. To find them, we need to filter out noise. So, we need to know what to look for.

The pictures are from here:

• Michael I. Cohen and Jeffrey D. Kaplan and Mark A. Scheel, On toroidal horizons in binary black hole inspirals, Phys. Rev. D 85 (2012), 024031.

### Part 4

Let’s imagine an old, advanced civilization in the doomed galaxy PG 1302-102.

Long ago they had mastered space travel. Thus, they were able to survive when their galaxy collided with another—just as ours will collide with Andromeda four billion years from now. They had a lot of warning—and so do we. The picture here shows what Andromeda will look like 250 million years before it hits.

They knew everything we do about astronomy—and more. So they knew that when galaxies collide, almost all stars sail past each other unharmed. A few planets get knocked out of orbit. Colliding clouds of gas and dust form new stars, often blue giants that live short, dramatic lives, going supernova after just 10 million years.

All this could be handled by not being in the wrong place at the wrong time. They knew the real danger came from the sleeping monsters at the heart of the colliding galaxies.

Namely, the supermassive black holes!

Almost every galaxy has a huge black hole at its center. This black hole is quiet when not being fed. But when galaxies collide, lots of gas and dust and even stars get caught by the gravity and pulled in. This material form a huge flat disk as it spirals down and heats up. The result is an active galactic nucleus.

In the worst case, the central black holes can eat thousands of stars a year. Then we get a quasar, which easily pumps out the power of 2000 ordinary galaxies.

Much of this power comes out in huge jets of X-rays. These jets keep growing, eventually stretching for hundreds of thousands of light years. The whole galaxy becomes bathed in X-rays—killing all life that’s not prepared.

Let’s imagine a civilization that was prepared. Natural selection has ways of weeding out civilizations that are bad at long-term planning. If you’re prepared, and you have the right technology, a quasar could actually be a good source of power.

But the quasar was just the start of the problem. The combined galaxy had two black holes at its center. The big one was at least 400 million times the mass of our Sun. The smaller one was about a tenth as big—but still huge.

They eventually met and started to orbit each other. By flinging stars out the way, they gradually came closer. It was slow at first, but the closer they got, the faster they circled each other, and the more gravitational waves they pumped out. This carried away more energy—so they moved closer, and circled even faster, in a dance with an insane, deadly climax.

Right now—here on Earth, where it takes a long time for the news to reach us—we see that in 100,000 years the two black holes will spiral down completely, collide and merge. When this happens, a huge pulse of gravitational waves, electromagnetic radiation, matter and even antimatter will blast through the galaxy called PG 1302-102.

I don’t know exactly what this will be like. I haven’t found papers describing this kind of event in detail.

One expert told the New York Times that the energy of this explosion will equal 100 million supernovae. I don’t think he was exaggerating. A supernova is a giant star whose core collapses as it runs out of fuel, easily turning several Earth masses of hydrogen into iron before you can say “Jack Robinson”. When it does this, it can easily pump out 1044 joules of energy. So, 100 millon supernovae is 1052 joules. By contrast, if we could convert all the mass of the black holes in PG 1302-102. into energy, we’d get about 1056 joules. So, our expert was just saying that their merger will turns 0.01% of their combined mass into energy. That seems quite reasonable to me.

But I want to know what happens then! What will the explosion do to the galaxy? Most of the energy comes out as gravitational radiation. Gravitational waves don’t interact very strongly with matter. But when they’re this strong, who knows? And of course there will be plenty of ordinary radiation, as the accretion disk gets shredded and sucked into the new combined black hole.

The civilization I’m imagining was smart enough not to stick around. They decided to simply leave the galaxy.

After all, they could tell the disaster was coming, at least a million years in advance. Some may have decided to stay and rough it out, or die a noble death. But most left.

And then what?

It takes a long time to reach another galaxy. Right now, travelling at 1% the speed of light, it would take 250 million years to reach Andromeda from here.

But they wouldn’t have to go to another galaxy. They could just back off, wait for the fireworks to die down, and move back in.

So don’t feel bad for them. I imagine they’re doing fine.

By the way, the expert I mentioned is S. George Djorgovski of Caltech, mentioned here:

• Dennis Overbye, Black holes inch ahead to violent cosmic union, New York Times, 7 January 2015.

### Part 5

When distant black holes collide, they emit a burst of gravitational radiation: a ripple in the shape of space, spreading out at the speed of light. Can we detect that here on Earth? We haven’t yet. But with luck we will soon, thanks to LIGO.

LIGO stands for Laser Interferometer Gravitational Wave Observatory. The idea is simple. You shine a laser beam down two very long tubes and let it bounce back and forth between mirrors at the ends. You use this compare the length of these tubes. When a gravitational wave comes by, it stretches space in one direction and squashes it in another direction. So, we can detect it.

Sounds easy, eh? Not when you run the numbers! We’re trying to see gravitational waves that stretch space just a tiny bit: about one part in 1023. At LIGO, the tubes are 4 kilometers long. So, we need to see their length change by an absurdly small amount: one-thousandth the diameter of a proton!

It’s amazing to me that people can even contemplate doing this, much less succeed. They use lots of tricks:

• They bounce the light back and forth many times, effectively increasing the length of the tubes to 1800 kilometers.

• There’s no air in the tubes—just a very good vacuum.

• They hang the mirrors on quartz fibers, making each mirror part of a pendulum with very little friction. This means it vibrates very well at one particular frequency, and very badly at frequencies far from that. This damps out the shaking of the ground, which is a real problem.

• This pendulum is hung on another pendulum.

• That pendulum is hung on a third pendulum.

• That pendulum is hung on a fourth pendulum.

• The whole chain of pendulums is sitting on a device that detects vibrations and moves in a way to counteract them, sort of like noise-cancelling headphones.

• There are 2 of these facilities, one in Livingston, Louisiana and another in Hanford, Washington. Only if both detect a gravitational wave do we get excited.

I visited the LIGO facility in Louisiana in 2006. It was really cool! Back then, the sensitivity was good enough to see collisions of black holes and neutron stars up to 50 million light years away.

Here I’m not talking about supermassive black holes like the ones in the doomed galaxy of my story here! I’m talking about the much more common black holes and neutron stars that form when stars go supernova. Sometimes a pair of stars orbiting each other will both blow up, and form two black holes—or two neutron stars, or a black hole and neutron star. And eventually these will spiral into each other and emit lots of gravitational waves right before they collide.

50 million light years is big enough that LIGO could see about half the galaxies in the Virgo Cluster. Unfortunately, with that many galaxies, we only expect to see one neutron star collision every 50 years or so.

They never saw anything. So they kept improving the machines, and now we’ve got Advanced LIGO! This should now be able to see collisions up to 225 million light years away… and after a while, three times further.

They turned it on September 18th. Soon we should see more than one gravitational wave burst each year.

In fact, there’s a rumor that they’ve already seen one! But they’re still testing the device, and there’s a team whose job is to inject fake signals, just to see if they’re detected. Davide Castelvecchi writes:

LIGO is almost unique among physics experiments in practising ‘blind injection’. A team of three collaboration members has the ability to simulate a detection by using actuators to move the mirrors. “Only they know if, and when, a certain type of signal has been injected,” says Laura Cadonati, a physicist at the Georgia Institute of Technology in Atlanta who leads the Advanced LIGO’s data-analysis team.

Two such exercises took place during earlier science runs of LIGO, one in 2007 and one in 2010. Harry Collins, a sociologist of science at Cardiff University, UK, was there to document them (and has written books about it). He says that the exercises can be valuable for rehearsing the analysis techniques that will be needed when a real event occurs. But the practice can also be a drain on the team’s energies. “Analysing one of these events can be enormously time consuming,” he says. “At some point, it damages their home life.”

The original blind-injection exercises took 18 months and 6 months respectively. The first one was discarded, but in the second case, the collaboration wrote a paper and held a vote to decide whether they would make an announcement. Only then did the blind-injection team ‘open the envelope’ and reveal that the events had been staged.

Aargh! The disappointment would be crushing.

But with luck, Advanced LIGO will soon detect real gravitational waves. And I hope life here in the Milky Way thrives for a long time – so that when the gravitational waves from the doomed galaxy PG 1302-102 reach us, hundreds of thousands of years in the future, we can study them in exquisite detail.

For Castelvecchi’s whole story, see:

• Davide Castelvecchi Has giant LIGO experiment seen gravitational waves?, Nature, 30 September 2015.

For pictures of my visit to LIGO, see:

• John Baez, This week’s finds in mathematical physics (week 241), 20 November 2006.

For how Advanced LIGO works, see:

• The LIGO Scientific Collaboration Advanced LIGO, 17 November 2014.

### References

To see where the pictures are from, click on them. For more, try this:

The picture of Andromeda in the nighttime sky 3.75 billion years from now was made by NASA. You can see a whole series of these pictures here:

• NASA, NASA’s Hubble shows Milky Way is destined for head-on collision, 31 March 2012.

Let’s get ready! For starters, let’s deal with global warming.

### 13 Responses to Tale of a Doomed Galaxy

1. allen says:

If the smaller BH is moving at $c/100$ in an orbit that last 4 years then doesn’t that mean that the radius of that orbit is $c/100 \times (4 \textrm{years})/(2 \pi)$? If so, the radius is equal to 402.6 AU which is about 20 times Pluto’s orbital radius.

• John Baez says:

According to Wikipedia:

The two supermassive black holes are merging, and are 180 billion miles (2.9×1011 km) apart, comparable to the separation between the Sun and the Oort Cloud in our Solar System.

That’s about 1900 AU. I’ll let someone else figure out what’s causing the discrepancy here. The orbital period is directly observed and it’s probably correct within 50% or better. The distance can only be estimated, since we don’t know the angle of view (one black hole could be almost in front of the other). The masses and velocities are probably just guessed/inferred from the other data.

2. allen says:

Also, why should a BH merger release any energy other than gravitational energy and what quota of Hawking radiation a BH of their sizes must emit? Have event horizons become permeable?

• John Baez says:

A black hole merger emits mostly gravitational radiation, and it’s an interesting puzzle to figure out how destructive—or not—this radiation will be when the two black holes in PG 1302-102 collide and emit 1052 joules of gravitational radiation: 100 million supernovae’s worth of energy.

The jets emitted by the accretion disk of these black holes may go crazy as well during the collision: as the black holes spiral in, more matter may fall in as well. This could by itself be quite dramatic, even though the total energy involved is much less.

As for your last question, I mentioned that it seems one expert estimates that the merger of these black holes will turn approximately 0.01% of their combined mass into energy. In the long run, Hawking radiation turns all the mass into energy—but that’s an insanely slow process.

3. arch1 says:

If the putative civilization is very capable, but also – ahem – very prone to procrastination, could the collision prediction/retrodiction/whatever-you-call it conceivably prove false?

(OK I don’t really believe procrastination plays a role, but – morphing the Q a bit – I do wonder at what point during such a system’s evolution one can say that collision is absolutely inevitable despite all physically possible natural or artificial interventions. Is that simply the time at which the event horizons first make contact?).

• John Baez says:

I can’t quite answer either of your questions, but here’s what comes to mind:

1) A strange thing about the concept of event horizon is that the location or even existence of an event horizon ‘now’ can depend on our actions ‘in the future’. I’m putting in quotes because the concepts of ‘now’ and ‘future’ are tricky in general relativity. But that’s not really the problem here. The event horizon is defined to be the imaginary surface such that light emitted within this surface can never get out to infinity in the future. So, if we were able to drag black holes around or create them by compressing matter, the location of the event horizon now might depend on what we do in the future.

However, what we do might have just a tiny effect.

2) Regarding procrastination: there’s a sense in which we’ve already started procrastinating in our response to the Milky Way’s collision with Andromeda. We feel sure it’s going to happen, yet we’re not doing anything about it—not even planning.

• arch1 says:

#1: Thank you, fascinating. #2: I for one am preparing by watching Gale Sayers highlights on YouTube:-)

4. arch1 says:

“One expert told the New York Times that the energy of this explosion will equal 100 million supernovae.”

This makes supernovae seem positively piddling by comparison – and they are, but only by comparison. They are decidedly non-piddling with respect to normal human scales. Those who, like me, may need convincing on this point, should read the answer to the below question, taken from this very entertaining xkcd What’s Next:

“Which of the following would be brighter, in terms of the amount of energy delivered to your retina:
1. A supernova, seen from as far away as the Sun is from the Earth, or
2. The detonation of a hydrogen bomb pressed against your eyeball?”

• John Baez says:

Yes, a supernova is an utterly amazing event. But a hypernova is even more amazing. From Week 204 of This Week’s Finds.

The life of a star is largely determined by its mass. Small stars last a long time and fade away inconspicuously, while big stars live fast and die with a bang. Wolf-Rayet stars are among the biggest, about 60 times as heavy as the Sun. Like the sun, they begin life as cloud of gas that collapses and heats up until the hydrogen in its core “catches fire” and starts fusing into helium, like a gigantic H-bomb held together by its own gravity. The core is surrounded by a envelope of cooler gas that transmits energy to the surface by convection and radiation, but doesn’t actually do any fusion itself.

This stage of a star’s life is called the “core burning phase”. But after a while helium builds up and sinks to the center, forming an inert helium core, with all the fusion going on in the layer of hydrogen right next to the core. This is called the “shell burning phase”.

What next? Well, for the Sun, as its hydrogen gradually runs out it’ll become a “red giant”, expanding to engulf the Earth… while meanwhile its helium core shrinks to a ball twice the size of the Earth and about 100 times the density of water, turning from ordinary plasma into something called a “degenerate electron gas”, where the Pauli exclusion principle limits further compression. As the core shrinks it’ll heat up, and when it reaches a temperature of 100 million kelvin the helium will catch fire and start fusing – mainly into carbon. Models predict that this happens in a runaway reaction called the “helium flash”, which puts out about 100 billion times the power of the present-day sun for a few hours – zounds! – but gradually settles down into a more stable phase of helium burning that lasts for tens of millions of years. During this phase, the Sun will not be a red giant anymore, but instead a hotter “yellow giant”.

The Sun will never get hot enough to burn elements heavier than helium, so eventually it’ll develop an inert core of carbon and other junk, surrounded by a helium burning shell, surrounded by a hydrogen burning shell. Then the outer layers will peel off and expand to form a huge nebula, leaving the core as a tiny “white dwarf”… which will cool, after eons, to a “black dwarf”.

Bigger stars do more exciting things. In particular, stars heavier than about 5 solar masses undergo a “carbon flash” when the carbon-rich core reaches 600 million kelvin and starts fusing into heavier elements. Heavier stars then go on to an oxygen-burning phase. Even heavier ones go on to a silicon-burning phase.

But when silicon fuses, it forms highly stable nuclei like iron that don’t want to fuse any further. So, silicon burning is the end of the line. And it doesn’t last long! For example, a star 25 times the mass of the Sun is expected to spend about 5 to 10 million years burning hydrogen, 0.5 to 1 million years burning helium, 500 to 1000 years burning carbon, 6 to 12 months burning oxygen… but just a day or so burning silicon!

Then what? Well, the details depend on the star’s mass. But when a star of at least 8 solar masses runs out of fuel, its core is made mainly of iron, and heavier than our Sun. When it cools, it reaches a point where all of a sudden it collapses – in about a tenth of a second. When it crashes in on itself, it gets so hot that the iron nuclei disintegrate and the whole mess explodes in a “type II supernova”. The star’s outer layers get thrown off at high speeds, while the core itself gets crushed into a neutron star… or, for truly heavy stars, a black hole!

Type II supernovae are among the most violent events in the cosmos. They can easily reach a temperature of about 50 billion kelvin and emit 1046 joules of energy, which is what our galaxy puts out in 10 years! 99% of this energy is in the form of neutrinos, emitted when protons in the iron core absorb electrons and turn into neutrons. But, the remaining 1% in the form of electromagnetic radiation is still enough to fry anything in the vicinity. The supernova in the Crab Nebula was about 6,300 light years away, but when its light reached us in 1054 AD, Chinese astronomers could see it in the daytime for 23 days!

You may think I’ve forgotten about GRB030329 and Wolf-Rayet stars, but I haven’t. This big digression was just to set the stage. I’ve sketched what stars of up to 25 solar masses will do, but remember, Wolf-Rayets are a lot bigger: they begin life at about 60 solar masses. And astronomy resembles opera in this way: the bigger the star, the more noise they make in their final scene. So, the stuff about supernovae was just to whet your appetite.

5. arch1 says:

Thanks John (also to the pointer to your vast archives). I didn’t know about hypernova/GRB connection. I wonder if observers can tell which burning mode a given star is in, and if so whether the modes are seen in anything like the expected ratios given their durations and other parameters. Maybe most are too rare to be amenable to such statistical tests.

Speaking of rare, your mention of GRB030329 reminded me of GRB080319B, which packs considerable human interest for something so remote and boringly-named.

I knew already that it was, for 30 seconds in 2008, the most distant (light travel time ~7.5B years) naked eye observable object ever detected. I now see that it was also the intrinsically brightest object ever detected, that this is due to its narrow (0.4 degrees) inner jet pointing our way, that its peak brightness occurred within hours of Arthur C. Clarke’s death, and that the ‘B’ in its name indicates that it was the second of an unprecedented five GRBs observed that day. Our wakes should all be that well-planned:-)

6. We mortals must stand if awe of experimental physicists and what they can do. If I perform a measurement which is accurate to 1 part per billion I think I am having a great day. to put this in some perspective, I spend time measuring acceleration, about 10 newtons here at my desk. If a nice light, empy 747 flies over head at its crusing altitude of 40000 feet it produces a contrary force of about 1 part per trillion of that (1e-13 Newtons, If I did my maths right). In fact, if a nice light fella of 50 kg happens to be flying around in orbit 10000 kilometers overhead (I hope you are okay person. the view must be amazing), I gather they will produce a force 3 times greater than 1e-28.

Do you know what the signal is expected to look like? Is it a sine wave, or a square wave? Do you know the frequency? Or is it more of a pulse.

• John Baez says:

Rob wrote:

Do you know what the signal is expected to look like?

Huge amounts of work have been expended to answer this question very precisely, so that people can filter out noise and look for signals of the expected shape in data from LIGO and other gravitational wave detectors. In 1997, the National Science Foundation gave a “Grand Challenge” grant to a big team of researchers to numerically simulate black hole collisions and the gravitational waves these would create. It turned out to be a lot harder than they’d expected! For a while people were worried that we’d be getting data but not know how to analyze it. Now, however, people are succeeding.

Instead of showing you what the signal looks like, I’ll suggest that you listen to it. This sound file illustrates the gravitational radiation produced a 10 solar mass black hole spiraling into a rapidly spinning million solar mass black hole. It’s sped up by about a factor of 1000 from reality. It’s quite dramatic near the end!