Gravitational Wonders, Fast Radio Bursts & Your Questions Answered

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Andrew Dunkley: Hello, once again, thanks for joining us on yet another

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edition of Space Nuts, or more common

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than a daily breakfast. Uh, my name is Andrew

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Dunkley. It is great to have your company. Uh, this

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is a Q and A edition, and that means, uh,

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we only use two letters of the Alphabet.

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Uh, but, uh, we also answer questions from the

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audience. Uh, Tony wants to know about binary

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planets and moons. Are there such things?

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Uh, Kevin asks, can light last

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forever? Alan wants, uh, to talk about,

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um, a story that we did do not so long

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ago. The strongest fast radio burst ever

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recorded. And Rennie is back with

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vertical oceans. That's all coming up

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on this episode of space nuts.

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Generic: 15 seconds. Guidance is internal.

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10, 9. Uh, ignition

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sequence start. Space Nuts 5, 4,

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3, 2. 1. 2, 3, 4, 5, 5, 4,

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3, 2, 1. Astronauts

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report it feels good.

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Andrew Dunkley: Joining us once again to unravel all of that

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is Professor Fred Watson Watson, astronomer at large. Hello,

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Fred Watson.

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Professor Fred Watson: Andrew. Good to see you again. What a surprise.

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Andrew Dunkley: Yes, indeed. It's good to see you, too. I

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actually got to see your office for real the other day, which is

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nice. Yeah.

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Professor Fred Watson: And you couldn't believe how small it is.

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Andrew Dunkley: That's the thing about, uh, cameras in general.

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They tend to make things look much, much bigger than they really

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are.

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Professor Fred Watson: Um, um, but, well, ah, yes, it's in. It's big enough.

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But, yes, it's.

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Andrew Dunkley: It does the job. I mean, mine's probably

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a bit smaller than yours by the look.

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Professor Fred Watson: There you go. Yes.

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Andrew Dunkley: Um, now, uh, we should get straight to business. Uh,

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we've got, uh, four questions to tackle today, all

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text questions. And while I'm at it, I will send out

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an appeal for new questions. We're running short.

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Um, we sort of threw some together the other day

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because I didn't have much to work with when I got back

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because I had completely erased everything that I had

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done and left it all to you and Heidi. But, um,

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now I need some stuff. So send us some

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questions via our website, spacenutspodcast.com or

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spacenuts IO audio or text?

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We don't mind which. And, uh, yeah, we'll get

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stuck into them.

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Um, now, Fred Watson, question one.

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Hi, Fred Watson. Andrew and or Heidi, Love the

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podcast. Keep up the good work, dad jokes and bizarre

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background animal noises.

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Congratulations on being. Wait for this, Fred Watson.

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Congratulations on being the seventh biggest,

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uh, astronomical show.

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Seventh biggest.

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Professor Fred Watson: We were,

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um, seven out of the top 50. Yeah.

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Andrew Dunkley: Yeah, I thought there were only eight. Anyway, carry

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on.

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Uh, Tony says the podcast often talks about binary

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stars, but can planets and moons also

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form in a paired configuration? Could this

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happen or would competing gravitational forces

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from larger mass objects make it impossible?

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I presume that as we haven't found any

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binary planets or moons amongst the myriad

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satellites in the solar system, that it's very unlikely.

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But is it impossible? That comes from

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Tony in Scotland. He's 20 minutes from

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St Andrews. He thought you'd like to know that.

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Professor Fred Watson: Yeah, that's lovely. Indeed. Uh,

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Saint Andrews is right behind me on the wall.

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That 17th century map there.

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Andrew Dunkley: Yes, yes, I see that. Nice.

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Professor Fred Watson: Um, so, uh,

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yeah, the answer is yes. Um, now

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clearly planets can form moons. We've got

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one. And most of the other planets actually, uh,

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Mercury and Venus don't have moons, but all the rest do.

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Um, but I think that's not what, um, uh,

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Tony's asking about. Uh, it's

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about, you know, the idea of things

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forming in pairs like,

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like binary stars where you've got two stars

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which might have fairly comparable masses and

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orbit around a, um, you know, a common

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centre of mass. Yeah. Uh, which we call the

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barycenter. So, um,

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yes, uh, objects, stars. We

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think actually stars form more commonly in pairs than singly,

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which is quite interesting because we don't. The sun doesn't

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have a binary companion. Got lost a few

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billion years ago and we still don't know where it is. Uh,

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that's one of the things that people actually look for.

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Sun's sibling star one that's got identical

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chemistry to the sun. There's a few

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candidates. Anyway, uh, can planets do

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that? Uh, and the answer is yes. Um,

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uh, and in fact it's not just

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planets, but the smaller,

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uh, bodies of the solar system perhaps

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more readily form in binaries,

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uh, as pairs. Uh, and,

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uh, the kind of classic example of

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this, um, is when we look

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at many asteroids, not all of

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them, but many of them are shaped like

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peanuts in, you know, a peanut shell

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because they've got two lobes to them, two blobs

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which are stuck together. And that's thought to be

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because, uh, they formed as a pair of

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objects, uh, and gradually

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spiralled together, not colliding,

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but in a fairly gentle, um,

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coming together, uh, where basically

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they. Gravity just pulls them together and they stick together and

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they often form a region around the

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join, if I can put it that way, where material

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tumbles down from the surface and collects in

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that area. And you've only to think of some of the best known ones,

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like, um, uh. Do you remember

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Arrokoth? We thought it was a snowman

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in the deepest depths of the solar

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system. Um, it's actually two pancakes Joined up

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effectively. But that's, that's a binary object.

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Um, you and I spoke um, uh

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back in the um, mid 20

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mid 2010s I think

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about um, the comet known

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as Churyumovka, Otherwise known as

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67p which looked like a rubber duck. And that's

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because it had two lobes as well, a big one and a small one.

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So that two lobe um situation

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very common among the smaller objects in the

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solar system. Uh probably

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binary systems that have come together. Not

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only that, we know of many uh

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asteroids that have moons, um and perhaps the

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best known uh, and certainly as far as space

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nuts is concerned is that pair known as

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Didymos and Dimorphos, uh

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which are uh, the pair of asteroids

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that the DART spacecraft targeted a

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few years ago. Dart uh,

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clouted uh Dimorphos uh

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firmly in its face, uh at a speed of

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6 kilometres per second, half tonne uh of

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material and changed its orbit around the

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uh, around Didymos by no fewer

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than 30 minutes. It was quite a

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successful venture. Um, so

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that's all telling you that there's pairs of objects

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are very, very common. Um

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and I suppose the best example

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of what you might call a binary planet because a binary

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planet you'd expect the two masses to have roughly

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equal or similar characteristics.

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Uh but the dwarf planet Pluto and its

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uh, satellite Charon, uh, I think

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Charon is half the diameter of Pluto if I remember

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rightly. It's quite large compared with Pluto

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and they orbit around their common centre of Pluto

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mass, the barycenter. So uh,

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the kind of informal definition of a binary

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object um is when the

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centre of mass of the two halves of it

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are uh, is outside either

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body if I can put it that way. So the centre of mass is

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somewhere in the space between them rather than being inside

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as the centre of mass of the Earth and Moon

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is actually inside the Earth which is why we consider

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the moon to be a satellite and not really a binary

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object. Making sense there.

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Um, that's basically the story. It's a very

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common phenomenon.

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Andrew Dunkley: Could it work for

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planets the size of ours though? Let's say Venus was

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out here. Could we

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sort of get into that kind of dance with Venus because they're

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similar sized planets. Similar, similar mass.

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Professor Fred Watson: They are, that's right. And um,

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I'm sure it's not impossible

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that a situation like that might

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arise. I suspect why it

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doesn't is it's linked with

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the way we define a planet Andrew.

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Uh, because to be a planet an object's got

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to have pulled itself into a spherical shape, but it's

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also got to have cleared all the debris around it.

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Um, and that's the process of

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accretion. That's gravitational

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sweeping up of the material within

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the old protoplanetary disc that used to

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be around the sun but is now the planets. Uh, and

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so I suspect that that process itself

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perhaps favours, um,

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single objects, because anything that looks as though

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it's going to be another object the same size

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will get swept up by, uh, one. One or the other. There'll be

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one of them that turns out to be dominant. And it's

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possible that that's why we see the planets

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singly, because they're big and they've swept up the material

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around them. Whereas when we look at the aster

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moons and things like that, dwarf planets like Pluto,

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um, uh, you might find binary objects are

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much more common, uh, because there hasn't been that

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gravitational cleaning up of. Of their environment, if

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I can put it that way. Yeah. So I suspect that's the way it works.

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Andrew Dunkley: That makes sense. Very good.

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All right, so, Tony, it's taken us 10 minutes to tell

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you. Yes.

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Professor Fred Watson: Sorry about that, Tony, but. Yes, but

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great. Give my love to Saint Andrew.

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Andrew Dunkley: Yes, yes. He says he's from darkest

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Fife.

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Professor Fred Watson: Well, Fifes, Um,

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it'll be dark soon when we get to

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the winter solstice in the northern hemisphere. But it is a very,

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very pretty part of the world.

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Um, in fact, it was. It

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might have been. James, one of the early kings

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of Scotland, described it as a

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beggar's mantle. Uh, what was it? A

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beggar's mantle fringed with gold. And what

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he was referring to is that it's this green

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landscape, uh, with a lot of agriculture.

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Fields are like a beggar's, uh. A beggar's

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scarf, which is bits of material sewn together

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and fringed with gold because it's got golden beaches all the way around

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it.

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Andrew Dunkley: Nice. Very nice.

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Professor Fred Watson: Yeah. It's a great place.

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Andrew Dunkley: Yeah. Thanks, Tony. Thanks for your question.

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Next one comes from Kevin.

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Professor Fred Watson: Hello.

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Andrew Dunkley: I love your show. And please keep Heidi coming back, even

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as a guest host with both of you.

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We're actually talking about that, uh, the three of you would be

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great together. Oh, that's nice. Uh, my question

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is, if the universe is 13 and a half

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or so billion years old, uh, how

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long before we stop seeing the light from 13 and

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a half billion years ago? It seems that every

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20 or 30 years we launch a new telescope and it keeps being

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able to see further and further back, but eventually the light

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that's 13 billion years old will have to be 4

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billion years old. Uh, the light can't keep

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lasting forever, can it? Uh, I hope

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I'm clear enough. I know they say the universe

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is expanding out to 46 billion light years.

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But uh, we don't know for sure because we

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can't see beyond the cosmic microwave background.

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Thank you. From Kevin. It's a good question.

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We have talked about the life of light.

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Um, that's a good title for a book. The life

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of light before.

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And I think you did say it does have

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a um, you know, a

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termination age. Uh,

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sometimes light ends where it hits something

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or and it turns into something else. But um,

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yeah, I can't remember.

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Professor Fred Watson: But yeah. So actually it, if it

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doesn't hit something, it does pretty well go on forever. Is that

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true? Yeah, um,

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and it is sort of

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counterintuitive. We tend to think things that go on

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forever, something wrong with them.

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Um, but uh, electro.

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It's not just light, it's electromagnetic radiation.

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Uh, it, it basically keeps going to

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infinity. Now it might get very very weak.

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Um, because of the inverse square rule. Every

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uh, as the distance doubles the um,

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you know the intensity goes down by a factor of four because it's the

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square of the distance. Um,

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but uh,

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the, the question that, that Kevin poses,

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uh, is, is an interesting one. I

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mean uh, where it's absolutely true

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that we are seeing the flash of the Big Bang when we look at

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the cosmic microwave background radiation.

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Um, exactly as he says, we can't see beyond that.

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So we see that as

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um, brightness of the sky in

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microwaves, radio waves that is

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everywhere in the sky and it's almost completely

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uniform. It's not quite. And it's just as well because that

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uh, non uniformity is caused by

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the sound waves within the Big Bang plasma

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which eventually uh, is what gave rise to

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galaxies and stars and all the rest of it. We think

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so. Um, so yes, we're so we're looking

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at a, a boundary

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uh, beyond which we can't see. And so

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I think um, just

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clarifying uh, Kevin's comment,

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um, that 46 billion light

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years is probably what we call the

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proper radius of the universe. In

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other words, it's the radius of the universe if we could see it

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all. But we can't because we're always looking back in

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time. So we tend to talk about uh, co.

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Moving universe

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looking back at a time time. Um,

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if we think in terms of look back times rather than in terms

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of distances. That's the short answer.

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So I'll look back time to the cosmic

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microwave background radiation is 13.8 billion years.

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Um, but the universe probably goes on a lot further

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beyond that, exactly as Kevin said. So we can't really

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define its size. Uh, but

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what is interesting is that that boundary,

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that cosmic microwave background boundary,

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is actually receding from us at speed of

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light. Uh, and,

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um, I, uh, won't go into the details of why we know that, but

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it is. It's moving away from us at the speed of light, but it,

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but it's still. The light that it has emitted

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is still going on through the universe and will continue to

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do so. Uh, eventually, as the universe expands,

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it'll get very weak, particularly if it turns out that dark energy

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just keeps on, uh, going. Uh, there's

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new evidence that suggests that dark energy is, is

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reducing. Uh, which might mean that one day there

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is a turnaround and we might one day

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be back to the Big Crunch idea that we had in the

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1970s. Or the Gnab Gibbers, uh, as

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Brian Schmidt calls it, so.

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Andrew Dunkley: Or the, or the Big Crack.

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Professor Fred Watson: Well, the Big Crack could be if it keeps on expanding. Yeah,

335
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the Big Rip, where space itself just tears

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apart. I, um, think that's a weird

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quantum phenomenon that I'm not going to get into now. But,

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um, something to look forward to anyway in the distant future.

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Andrew Dunkley: Yes, yes, we can

340
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wait. We usually say we can't wait. We can't wait

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to examine the samples from Mars. But we can

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wait for the Big Rip. Or the Gnab Gib.

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Definitely no hurry for that. Uh, thank

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you, Kevin. Lovely to hear from you. And this

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is Space Nuts Q A edition with Andrew

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00:16:14.900 --> 00:16:17.500
Dunkley and Professor Fred Watson Watson.

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Generic: Roger, your lot is right here.

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Professor Fred Watson: Also Space Nuts.

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Andrew Dunkley: Our next question comes from Alan. He's in San

350
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Antonio, Texas. Recently, I was listening to

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another podcast where they talked about a news

352
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story about the strongest fast radio burst

353
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ever recorded. Yes, we have talked about that before.

354
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Uh, it's not an astronomy or science podcast, so,

355
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uh, they'll not be able to answer my question.

356
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And he thinks we can, Fred Watson.

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Professor Fred Watson: Anyway, we can put him right.

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Andrew Dunkley: They mentioned that most fast radio bursts

359
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were from billions of light years away. My first

360
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thought was, hold on. If we don't know the

361
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cause of FRBs, how can anyone know

362
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the distance to the source? Hopefully Fred Watson can answer

363
00:17:04.380 --> 00:17:07.260
that. Then maybe Fred Watson will talk about the news item.

364
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If I heard right, the, FRB that, uh,

365
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it was talking about is intrinsically the brightest

366
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ever, and it was in the Milky Way.

367
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Uh, if that is the case, then it's apparent brightness must

368
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have been so powerful that it saturated the instruments on the

369
00:17:22.100 --> 00:17:25.100
telescope. That comes from Alan in Texas. Yeah, we

370
00:17:25.100 --> 00:17:28.050
spoke about that when it was first uh, published. The uh,

371
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findings. First published. Yeah, the um, the, the

372
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brightest um, ever fast radio

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burst or something to that effect. Uh, so we probably should talk

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about that first before we um,

375
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answer the first part of the question.

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Professor Fred Watson: Yeah, the goat, wasn't it greatest of all

377
00:17:45.360 --> 00:17:46.200
time? Yes,

378
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but I think we're talking about two different things because,

379
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um, if you have the

380
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intrinsically greatest of all

381
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time within our own Milky Way, don't

382
00:18:00.120 --> 00:18:02.860
get fried. I think, um. Whoops. Uh,

383
00:18:03.160 --> 00:18:05.560
or at least as exactly as.

384
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As Alan says it would fry the instruments

385
00:18:09.120 --> 00:18:11.720
on the telescope. Exactly right. There

386
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certainly have been, um,

387
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FRBs which

388
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uh, which come from our galaxy.

389
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Um,

390
00:18:23.530 --> 00:18:26.330
they're, they're thought to be flares

391
00:18:26.330 --> 00:18:29.250
on magnetars. Uh, a magnetar is

392
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a highly magnetic neutron star.

393
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Intense magnetic fields, sort of unbelievably

394
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intense. And eventually occasionally you get flares

395
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on these things which give you this very brief

396
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uh, burst of radio radiation which

397
00:18:43.530 --> 00:18:45.850
we call an frb, a fast radio burst.

398
00:18:46.640 --> 00:18:49.040
Um, but, but that was.

399
00:18:49.520 --> 00:18:52.480
So that was one that was not as powerful as the ones

400
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that we see deep in the universe. The goats. The greatest

401
00:18:55.440 --> 00:18:58.400
of all time. Um, so I'm, I'm m probably

402
00:18:58.400 --> 00:19:01.320
not covering that news item very well. Uh, but let

403
00:19:01.320 --> 00:19:03.960
me just briefly answer the first part of

404
00:19:03.960 --> 00:19:06.880
Alan's question. Um, if we don't know the cause

405
00:19:06.880 --> 00:19:09.720
of FRBs, how can anyone know the distance to the source?

406
00:19:09.720 --> 00:19:12.640
It's a great question. And um, that was

407
00:19:12.640 --> 00:19:15.360
one of the puzzles. In the early era

408
00:19:15.360 --> 00:19:18.200
of fast radio bursts, there were a lot of them were

409
00:19:18.200 --> 00:19:21.120
detected. They only happened once. There are a few repeating

410
00:19:21.120 --> 00:19:23.680
ones, uh, but

411
00:19:23.800 --> 00:19:26.400
um, most of them only happen

412
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uh, once. Um,

413
00:19:29.600 --> 00:19:31.600
what you have to do is,

414
00:19:32.200 --> 00:19:34.560
uh, when you detect one of these things,

415
00:19:35.040 --> 00:19:37.880
you have to use a radio telescope that is

416
00:19:37.880 --> 00:19:40.440
capable of pinpointing its

417
00:19:40.440 --> 00:19:43.320
direction with very high accuracy. And

418
00:19:43.320 --> 00:19:45.510
that's where ASCAP came in. The Australian,

419
00:19:46.380 --> 00:19:49.340
uh, um, Square Kilometre Array

420
00:19:49.340 --> 00:19:51.940
Pathfinder. Ascap, uh, which is a

421
00:19:51.940 --> 00:19:54.620
telescope in Western Australia. It's an array of 36

422
00:19:54.620 --> 00:19:57.620
dishes. Um, and because it's an

423
00:19:57.620 --> 00:20:00.500
array like that, it's very, very good at

424
00:20:00.500 --> 00:20:03.420
pinpointing where signals come from to a very high

425
00:20:03.420 --> 00:20:06.140
degree of accuracy. So if you could do that,

426
00:20:06.460 --> 00:20:09.300
and it took them a while to get that

427
00:20:09.300 --> 00:20:12.200
act together, but they did. Um, and what

428
00:20:12.200 --> 00:20:15.120
you can do is then take that position and

429
00:20:15.120 --> 00:20:18.120
look at that point with a visible light telescope.

430
00:20:18.760 --> 00:20:21.320
And uh, what was found

431
00:20:21.320 --> 00:20:24.120
consistently with fast radio bursts is yes,

432
00:20:24.200 --> 00:20:27.100
they come from distant galaxies. Uh,

433
00:20:27.530 --> 00:20:30.400
um, the puzzle was that they're not usually in the

434
00:20:30.400 --> 00:20:33.240
centre of these galaxies, which is where you expect all the high energy

435
00:20:33.240 --> 00:20:36.120
processes to take place because there's a supermassive black

436
00:20:36.120 --> 00:20:38.800
hole there. Often they're in the kind of suburbs of

437
00:20:38.800 --> 00:20:41.680
galaxies, which is one reason why we

438
00:20:41.680 --> 00:20:44.600
believe they're these magnetar flares because then

439
00:20:44.840 --> 00:20:47.720
they're not something associated with a, um, high energy

440
00:20:47.880 --> 00:20:50.520
supermassive black hole. They're associated with

441
00:20:50.680 --> 00:20:53.080
very compact stars. So

442
00:20:54.200 --> 00:20:56.440
if you can identify in a galaxy,

443
00:20:56.920 --> 00:20:59.520
then you can measure the redshift of the

444
00:20:59.520 --> 00:21:02.200
galaxy itself using an optical, a visible light

445
00:21:02.200 --> 00:21:05.080
telescope. That gives you the redshift which we equate to

446
00:21:05.080 --> 00:21:08.050
distance. Uh, so that's how we know where they are

447
00:21:08.050 --> 00:21:10.770
and how far away they are. And that's really,

448
00:21:10.930 --> 00:21:13.850
um, you know, one of the great stories of the, of

449
00:21:13.850 --> 00:21:16.210
the FRB saga that we have managed to

450
00:21:16.370 --> 00:21:19.330
pinpoint these brief flashes of radiation, they last

451
00:21:19.330 --> 00:21:22.250
a thousandth of a second at most, uh, and find

452
00:21:22.250 --> 00:21:24.770
out where they come from. And it's just because we can

453
00:21:24.770 --> 00:21:27.610
pinpoint their positions very accurately and then follow

454
00:21:27.610 --> 00:21:30.570
it up with optical or visible light telescopes. I have

455
00:21:30.570 --> 00:21:33.530
to say that one of the, um, uh,

456
00:21:33.660 --> 00:21:36.420
great collaborations uh, in that

457
00:21:36.420 --> 00:21:39.300
regard has been ascap, the Australian Square Kilometre

458
00:21:39.300 --> 00:21:42.220
Array Pathfinder, ah, uh, linking with

459
00:21:42.300 --> 00:21:44.820
the telescopes of the

460
00:21:44.820 --> 00:21:47.420
European Southern Observatory down in Chile, the optical

461
00:21:47.420 --> 00:21:50.420
telescopes, what we call the VLT, the Very Large Telescope,

462
00:21:50.420 --> 00:21:52.700
those four 8.2 metre

463
00:21:52.780 --> 00:21:55.580
telescopes that are so good at uh,

464
00:21:55.580 --> 00:21:58.460
measuring the distances to very distant objects. So

465
00:21:58.460 --> 00:22:00.150
that's been a really great collaboration.

466
00:22:00.620 --> 00:22:03.460
Andrew Dunkley: M. Now, um, you probably

467
00:22:03.460 --> 00:22:06.300
already answered this in the past and my brain won't let me

468
00:22:06.860 --> 00:22:09.660
find the answer, but what causes fast

469
00:22:09.660 --> 00:22:10.700
radio bursts?

470
00:22:10.940 --> 00:22:13.820
Professor Fred Watson: It's what we were saying, the idea of a flare

471
00:22:14.380 --> 00:22:16.820
taking place on the surface of a, ah, highly

472
00:22:16.820 --> 00:22:19.700
magnetised neutron star. Now we find

473
00:22:19.700 --> 00:22:22.580
that very hard to envisage because you and I have struggled

474
00:22:22.580 --> 00:22:25.540
to imagine what neutron stars are like when we

475
00:22:25.540 --> 00:22:28.380
know that they've got mountains on them that are a few millimetres

476
00:22:28.380 --> 00:22:31.300
high. Um, you know, um, what is

477
00:22:31.300 --> 00:22:34.200
the surface of an neutron star like? It's just, ah, it's

478
00:22:34.280 --> 00:22:37.120
impossible to imagine, um, and so it's kind of

479
00:22:37.120 --> 00:22:40.040
equally impossible to imagine a flare on one of these things

480
00:22:40.040 --> 00:22:42.680
that is so bright that it outshines the sun for

481
00:22:43.140 --> 00:22:45.920
um, you know, for a thousandth of a second or outshines the

482
00:22:45.920 --> 00:22:48.780
sun's entire radiation, uh, uh,

483
00:22:48.780 --> 00:22:51.600
history for a thousandth of a second. Amazing

484
00:22:51.600 --> 00:22:52.040
stuff.

485
00:22:52.200 --> 00:22:55.200
Andrew Dunkley: Extraordinary. Thanks for the question, Alan. Hope you're

486
00:22:55.200 --> 00:22:55.480
well.

487
00:22:57.960 --> 00:23:00.040
Generic: Zero G and I feel fine.

488
00:23:00.040 --> 00:23:01.000
Andrew Dunkley: Space nuts.

489
00:23:01.160 --> 00:23:03.950
And to our final question today from one of our regular

490
00:23:04.180 --> 00:23:06.940
contributors. Hi, Rennie. Uh, if I look at the

491
00:23:06.940 --> 00:23:09.700
Earth from the distance, let's say of Earth's

492
00:23:09.700 --> 00:23:12.660
moon and Earth is in a gravitational well,

493
00:23:13.380 --> 00:23:16.100
why aren't the vertical, uh, why aren't

494
00:23:16.100 --> 00:23:18.940
the vertical oceans on Earth that I'm looking

495
00:23:18.940 --> 00:23:21.900
at not dripping down the sides of the Earth towards

496
00:23:21.900 --> 00:23:24.420
the deepest parts of the gravitational well?

497
00:23:26.460 --> 00:23:29.380
Uh, I'm not sure he's serious. Maybe he is.

498
00:23:29.420 --> 00:23:32.400
Um, some people look at

499
00:23:32.400 --> 00:23:34.880
the planet and go, okay, it's a sphere, so why

500
00:23:35.360 --> 00:23:38.280
is everything staying where it is? Why, why wouldn't

501
00:23:38.280 --> 00:23:40.240
the water drip down.

502
00:23:40.560 --> 00:23:41.360
Professor Fred Watson: To the bottom

503
00:23:43.680 --> 00:23:46.320
a big puddle in Antarctica? Um,

504
00:23:46.640 --> 00:23:49.360
well, it, yes, it is in a gravitational well, but

505
00:23:49.360 --> 00:23:52.160
it's a three dimensional one. We, you know, we look at,

506
00:23:52.920 --> 00:23:55.520
uh, depictions of a gravitational

507
00:23:55.600 --> 00:23:58.520
well and it's a, it's like a trampoline.

508
00:23:58.520 --> 00:24:01.360
It's a surface with a dent in the

509
00:24:01.360 --> 00:24:04.240
middle where you've got planet

510
00:24:04.240 --> 00:24:07.240
Earth or whatever, uh, other gravitational objects,

511
00:24:07.660 --> 00:24:10.520
uh, we're talking about. Uh, so a gravitational

512
00:24:10.520 --> 00:24:12.999
well is, um, a good

513
00:24:12.999 --> 00:24:15.960
description because that's sort of what it looks like, except

514
00:24:16.760 --> 00:24:19.080
that it's a gravitational well in three

515
00:24:19.080 --> 00:24:22.000
dimensions, not two dimensions, as the surface

516
00:24:22.000 --> 00:24:24.760
of a trampoline is. Uh, so it's a three

517
00:24:24.760 --> 00:24:27.670
dimensional entity. And it turns out that the

518
00:24:27.670 --> 00:24:30.310
gravitational well is at the centre

519
00:24:30.550 --> 00:24:33.430
of any gravitating object like the Earth.

520
00:24:33.430 --> 00:24:36.390
So, um, yes, the oceans do drip

521
00:24:36.390 --> 00:24:39.190
down, but they drip down towards the centre of the

522
00:24:39.190 --> 00:24:42.070
Earth, which is where the gravitational well is,

523
00:24:42.640 --> 00:24:45.510
uh, because it's a three dimensional well, not a two

524
00:24:45.510 --> 00:24:48.510
dimensional one. I do love the idea of the

525
00:24:48.510 --> 00:24:51.190
oceans kind of running down the side though. It's quite

526
00:24:51.270 --> 00:24:53.430
nice to think about.

527
00:24:54.550 --> 00:24:57.180
Fortunately, fortunately not the way it is because

528
00:24:57.180 --> 00:25:00.060
the, uh, the whole thing exists in three dimensions

529
00:25:00.140 --> 00:25:02.980
and we've got, um, the centre of the Earth as being the bottom of the

530
00:25:02.980 --> 00:25:03.980
gravitational well.

531
00:25:04.220 --> 00:25:07.100
Andrew Dunkley: Indeed. Simple, uh, answer to that

532
00:25:07.100 --> 00:25:09.980
one, Rennie. So thanks for sending your question in and

533
00:25:09.980 --> 00:25:12.860
once again I'll appeal for new questions. If

534
00:25:12.860 --> 00:25:15.100
you'd like to send them into us, jump on our website.

535
00:25:15.580 --> 00:25:18.380
I'll just do a search for Space Nuts podcast

536
00:25:18.860 --> 00:25:21.800
on your search engine and uh, find us there and,

537
00:25:21.800 --> 00:25:24.780
uh, send us text or

538
00:25:24.780 --> 00:25:27.450
audio questions, uh, um,

539
00:25:27.800 --> 00:25:30.200
through the AMA tab up the top. And

540
00:25:30.840 --> 00:25:33.840
don't uh, forget to tell us who you are and where you're from. We always

541
00:25:33.840 --> 00:25:36.600
like to know that just so that we can spam you.

542
00:25:37.160 --> 00:25:37.420
Professor Fred Watson: Um.

543
00:25:39.880 --> 00:25:40.840
Andrew Dunkley: Yes, all right.

544
00:25:40.840 --> 00:25:41.720
Professor Fred Watson: Is that what it's for?

545
00:25:41.800 --> 00:25:43.480
Andrew Dunkley: No, of course not.

546
00:25:44.600 --> 00:25:47.400
Of course not. We only send spam to people who

547
00:25:47.400 --> 00:25:48.520
volunteer for it.

548
00:25:49.080 --> 00:25:50.120
Professor Fred Watson: Yes, that's right.

549
00:25:51.580 --> 00:25:54.440
Andrew Dunkley: Uh, thanks, Ronnie, Alan, Kevin and

550
00:25:54.440 --> 00:25:57.280
Tony for your questions today. And thank you, Fred Watson, as

551
00:25:57.280 --> 00:25:58.470
always. It's been great fun.

552
00:25:58.540 --> 00:25:58.780
Generic: Fun.

553
00:25:59.340 --> 00:26:02.300
Professor Fred Watson: It's, it's great to answer the, you know, questions

554
00:26:02.300 --> 00:26:05.220
like that or at least have a crack at answering them. They're, uh, always

555
00:26:05.220 --> 00:26:08.140
thought provoking. And, um, thanks to all our listeners. And thanks too

556
00:26:08.140 --> 00:26:10.140
to you, Andrew, for carrying the show forward.

557
00:26:10.460 --> 00:26:13.460
Andrew Dunkley: Oh, my pleasure. I enjoy it. It's great

558
00:26:13.460 --> 00:26:16.340
fun. And we'd thank Huw in the studio, except

559
00:26:16.340 --> 00:26:18.780
he didn't turn up today. He went for a swim

560
00:26:19.100 --> 00:26:21.700
and ended up in Antarctica. So,

561
00:26:21.700 --> 00:26:24.460
um, he

562
00:26:24.460 --> 00:26:27.310
loves it down there. He's, um. Yeah,

563
00:26:27.790 --> 00:26:30.590
he's a fun guy. Uh, and, uh, that's it

564
00:26:30.590 --> 00:26:33.510
from, uh, us for another week. We'll see you very soon on

565
00:26:33.510 --> 00:26:36.150
another edition of Space Nuts. And from me, Andrew

566
00:26:36.150 --> 00:26:37.710
Dunkley. Bye. Bye.

567
00:26:38.910 --> 00:26:41.710
Generic: You've been listening to the Space Nuts podcast,

568
00:26:43.310 --> 00:26:46.030
available at Apple Podcasts, Spotify,

569
00:26:46.270 --> 00:26:49.030
iHeartRadio or your favourite podcast

570
00:26:49.030 --> 00:26:51.870
player. You can also stream on demand at Bitesz.com Com.

571
00:26:51.870 --> 00:26:54.830
Andrew Dunkley: This has been another quality podcast production from

572
00:26:54.830 --> 00:26:55.590
Bitesz.com