Stellar Scrutiny: Space Debris, Venusian Mysteries & the Quest for Cosmic Life

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Heidi Campo: Welcome back to another fun and exciting Q and A

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episode of space nuts.

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Voice Over Guy: 15 seconds. Guidance is internal. 10.

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Ah. 9. Uh, ignition

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sequence start. Space nuts. 5, 4,

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

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4, 3, 2. 1. Space nuts.

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Astronauts report. It feels good.

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Heidi Campo: I am your temporary host this episode,

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filling in for your beloved Andrew Dunkley. And my

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name is Heidi Campo.

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Professor Fred Watson: And.

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Heidi Campo: And joining us today to answer all of your burning

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questions is the lovely Professor

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Fred Watson, astronomer at large.

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Hi, Fred. How are you doing?

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Professor Fred Watson: I'm, um, well, Heidi, thanks, and great to see you again.

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I'm, um, so happy that, uh, we, uh, have these

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conversations because it brings a new

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excitement to the whole idea of Space Nuts with,

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uh, your questions as well as mine.

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Heidi Campo: Absolutely. And I know you're going to have so much fun at your

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conference this week. Speaking of questions, you're going to

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probably be answering a lot of questions and giving

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a lot of questions yourself. Is there any talks you're

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really looking forward to?

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Professor Fred Watson: Oh, uh, yes, there is actually. There's one day, uh,

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tomorrow. And um, this is

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an afternoon when, uh, the people who are

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most directly involved with some of the projects that

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are going on in, um, Australian

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astronomy, they get a chance to give an update.

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Uh, and it's things like, uh, what's

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happening with the Square Kilometer Array Observatory, which is being

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built, uh, jointly in South Africa and in Australia.

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It's things like, well, the Vera, uh,

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Rubin Observatory that we've talked about already. We've

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got connections with that, all of those things. These are

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sort um, of almost like news reports from these various

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facilities. Uh, and there's a lot

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of big questions that we need to ask

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in Australia about where we go with our, uh,

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for example, our membership of some of the international, uh,

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observatory community. So, uh, that's the one that's

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going to be the highlight for me. That will be tomorrow afternoon.

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And I'll report back, no doubt, in our next issue

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of Space Notes.

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Heidi Campo: Oh, I can't wait to hear it. That sounds wonderful.

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Well, Lei, let's uh, go ahead and just jump right on into

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our questions then. We have, uh. It's

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kind of typical fashion. We have a couple written questions

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and we have a couple audio questions. And

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so I'm going to go ahead and read.

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And I did not say so because our next question's from

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Minnesota. It just came out that way. But our next

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question is going to be a written question. And this is from Greg

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from Minnesota. And Greg says, g', day,

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Space Nuts. I'm Greg from Minnesota and I have

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two questions for you. This week One,

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what, if anything, is being done about

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Kessler Syndrome? Are there any plans to

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test something to remove space debris?

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Question two. Why is Venus's

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atmosphere so thick? CO2 is

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more dense than N2, uh, and O2 in

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our atmosphere. But I've heard that even if

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you removed the CO2 from Venus's

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atmosphere, it would still be three times

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more dense. How can it hold such a thick

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atmosphere? Or is

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it the Earth that is the odd duck that has an unusually

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thin atmosphere for a planet our size?

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Professor Fred Watson: They're great questions, uh, from Greg.

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I'm going to do the easy one first,

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which is what's, uh, being done about the Kessler Syndrome?

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Well, the Kessler Syndrome, uh, uh, I'm sure

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most of our listeners know is that,

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uh, it's the potential for there being a

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kind of runaway collision process

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among orbital debris, uh, things that

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orbit the Earth, uh, particularly in

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low Earth orbit, which is getting very, very crowded.

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Uh, at the Moment There are 30,000 pieces,

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debris that are being tracked, and they're bigger than about 100

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millimeters across, um, but there are millions of

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smaller bits. And remember that everything's going around

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at 8km per second or thereabouts.

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Um, so, uh, it is,

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uh, potentially a very dangerous thing. If you got a

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big enough collision between two, say, two

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defunct, uh, rocket bodies, then the

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debris from that could, uh,

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have this sort of domino effect, uh,

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in basically filling space

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with debris. That's the Kessler Syndrome.

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Uh, and what's being done about it is, yes, the

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recognition that we, uh, do

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need to fix this because, uh, Earth orbit is becoming

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more and more crowded, uh,

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as time goes on and the more spacecraft that we launch.

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And, uh, there are something like 12,000 active

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spacecraft in orbit at the moment. Uh,

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those, uh, as the numbers increase,

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the risks increase that you will eventually have

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a Kessler Syndrome phenomenon, uh, and

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then it's too late. You've got space that's actually

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unusable, which is a horrible thought when we think of

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how much we need space and how much we use, uh,

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the facilities that come to us because of orbiting

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spacecraft. So, uh,

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there is, you know, in a regulatory sense,

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uh, there is now the need you have to show whenever

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you launch a spacecraft that, uh, it's going to be

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deorbitable. In other words, there's got to be a way of clearing it

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from, uh, low Earth orbit. Uh, plus

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there are missions being planned to actually

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remove some of the larger pieces of

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space junk by decelerating them so that they burn

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up in the Earth's Atmosphere. So a lot is happening,

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but, uh, it's a slow process and it's actually quite a

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difficult, ah, job.

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Moving on to Greg's second question, which has

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got my brain, uh, in a panic,

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um, because I'm going to front

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up here and say I don't actually understand this,

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but I'm not a chemist. Uh, so let

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me just tell you what the story is,

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as Greg says, uh, well, why is it

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Venus's atmosphere so thick? That's the easy part. Uh,

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because, uh, we have an atmosphere that

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is something like 96% carbon dioxide.

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Uh, whereas the carbon dioxide in

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Earth's atmosphere is measured in parts per million. It's much, much

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lower than that. Um, uh,

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so, uh, as he says, co, uh, two is more dense than

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uh, nitrogen and oxygen in our atmosphere. But

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I've heard that even if you removed the CO2 from Venus's

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atmosphere, it would still be three times more dense. How can it

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hold onto such a thick atmosphere? And I think

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you're right, Greg. Uh, all the

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stuff I've read about the atmosphere of Venus,

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and I've churned through this quite a bit recently,

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uh, implies, uh, exactly what

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you've said, that if you took away the carbon dioxide,

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what you'd be left with will be essentially,

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um, a nitrogen atmosphere,

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um, which is uh,

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not that different from Earth's because we have a

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nitrogen atmosphere which has

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uh, some oxygen there.

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Uh, I think. I can't remember. It's the exact

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percentage, something like 15%, I think,

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oxygen. Um, and so you've got an

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atmosphere that does look more like Earth's, but, uh,

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is still going to have three times the atmospheric pressure

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of Earth. And I have struggled to work

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out why that is. Um, I think

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it's probably due to differences

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between the planets themselves. They are very similar

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in size. In fact, Earth is slightly more

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massive than Venus. Um, but, uh,

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there may be issues to do with, for

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example, internal structure of these two

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planets that makes them different in

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terms of what their atmosphere would do.

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Uh, so it's a piece of work that I'm going to continue

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researching. Greg, thank you for pointing me in this

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direction because it's one that is intriguing me

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and annoying me that I can't immediately see,

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uh, the answer, the simple answer to your question.

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There may not be one. It might be far more complex than

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uh, uh, than uh, we're currently

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expecting. But we will keep on um, with this and

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no doubt talk about it again down the track.

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Heidi Campo: Thank you so much, Greg.

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Um, our next question is from our

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favorite father, son Duo

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from Portugal. And this is an audio

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question, so I'm going to give Fred a second to cue

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that up and we are going to play that question for

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you right now. You guys are going to be able to listen to their question

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and then Fred is going to answer it. So here we

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go.

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Andrew Dunkley: Hello again. Uh, this is Philippe, Henrique's

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father from Portugal. Um, I just

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got home from work. It's 9:30 in the

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evening here in Portugal and Henrique

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was awake, eagerly waiting for

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me to get back home because he wants to ask you another

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question instead of being asleep.

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Um, thank you so much for asking me these

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questions. He really loves it when you answer his

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questions. And um, he asked

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me to listen to your podcast every time it's available

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another episode. Uh, I just wanted to

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say thank you for

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entertaining his questions and um,

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I'll leave him to it.

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Hi again. Um, I have another question

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for you about stars and black holes.

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How can black hole star support the mass

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of the black hole in there or without

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collapsing? And um, can you

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please tell more about them, like

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do they can support planets,

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um, how are

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they created, etc.

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Thank you for answering my question.

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Heidi Campo: Bye bye. Uh, this kid's going to be the next Einstein.

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Professor Fred Watson: I think so too. Yeah. So thanks to

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Philippe for, um, uh,

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uh, letting Enrique stay up

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late enough to record a question for,

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um, uh, Space Notes. And they're great

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questions too. Um, I think,

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uh, as I understand it, Enrique, your question

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was how can a star,

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basically, what stops a star from turning

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into a black hole? Uh, how can a star

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be supported? And the answer

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is it's all about the, you know, the physics

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of, of the way stars work. Even stars like

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the sun, which is relatively modest in size, certainly

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isn't going to cause a black hole, um,

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to be formed when it dies finally and perhaps

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3, 4 billion years time. Um, but

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a star like the sun is a balance between

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the gravity that wants to pull everything to the

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middle. It's a blob of gas and

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gravity basically wants everything to sink to the middle.

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And if that, if that was the case, then it

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would turn into something not quite like a black hole. It would turn into

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a white dwarf star, which is similar to a

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black hole but not quite as compact. But what stops

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that, as the star is in its normal

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lifetime is the radiation

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that is being generated by the

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nuclear processes, basically the

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atoms being smashed together in the star

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center. So there's all this activity

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generating energy in the center of the star as

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radiation, that radiation pressure which is acting

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outwards, balances the gravity. Exactly.

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So it's a delicate balancing act,

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uh, where the gravity is, you

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know, the tendency of the star to collapse

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is actually inhibited or stopped

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by the, uh, radiation

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pressure coming from the nuclear reaction. So

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that's what happens in a giant star, perhaps

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10 times bigger than the sun, um,

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during its lifetime, most of its lifetime, that

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balancing act is keeping going.

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The outward pressure is stopping the gravitational

254
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collapse. But, uh, these massive stars

255
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burn up their hydrogen, which is the fuel that

256
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generates, uh, these reactions in

257
00:12:20.490 --> 00:12:23.050
the center. Uh, they burn the hydrogen up very

258
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quickly. And once that hydrogen is gone,

259
00:12:26.450 --> 00:12:29.370
then, um, basically, it's not

260
00:12:29.370 --> 00:12:31.810
quite as simple as this, but basically the energy

261
00:12:32.050 --> 00:12:34.850
switches off. So there's nothing to stop

262
00:12:35.450 --> 00:12:38.450
the star from collapsing. It simply collapses under its

263
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own gravity. And a star that's big enough will

264
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indeed collapse into a black hole. Um,

265
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slightly smaller stars collapse into something we call a

266
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neutron star, which is where the subatomic

267
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particles are all crowded together.

268
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Um, then a slightly

269
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smaller star than that will collapse, like our sun will, into a white

270
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dwarf star, which is where all the electrons are

271
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bunched together. Uh, neutron stars.

272
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And I'm just moving now to the second part of your

273
00:13:07.020 --> 00:13:10.020
question. At least one neutron star we know does

274
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have planets. Uh, and that is,

275
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uh, it's one of the first planets beyond the solar system that was

276
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discovered because we could see its effect

277
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on the neutron star. Uh, and so, uh, it

278
00:13:21.820 --> 00:13:24.660
is possible for a planet to survive that

279
00:13:24.740 --> 00:13:27.380
explosive, uh, ending of the star.

280
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Uh, that results in the core collapsing. Um,

281
00:13:30.460 --> 00:13:33.260
and, you know, quite often the outer layers are blown

282
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away as well because that collapse is very

283
00:13:35.740 --> 00:13:38.700
explosive. It sounds weird that something collapsing should

284
00:13:38.700 --> 00:13:41.620
cause an explosion, but that's what happens. So.

285
00:13:41.620 --> 00:13:44.380
Yeah. So, um, I hope that covers the etc in your

286
00:13:44.380 --> 00:13:47.260
question, Enrique, but that's basically

287
00:13:47.660 --> 00:13:50.620
what, uh, we know about the way black, um, holes form

288
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and about the way planets might survive

289
00:13:53.500 --> 00:13:56.460
being around a black hole. We don't know of any planets

290
00:13:56.460 --> 00:13:59.420
yet that are around black holes, but we do know that they're

291
00:13:59.420 --> 00:14:02.260
around neutron stars, which are not too different from a black

292
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hole.

293
00:14:03.860 --> 00:14:06.180
Heidi Campo: That's fantastic. Yeah. Please keep the

294
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curiosity going. Feed that kid whatever science

295
00:14:09.140 --> 00:14:12.100
he needs to keep fueling these questions,

296
00:14:12.100 --> 00:14:14.340
because this is really, really fun.

297
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Professor Fred Watson: Okay, we checked all four systems and game with a go.

298
00:14:19.820 --> 00:14:20.820
Space nets.

299
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Heidi Campo: Um, next question. There is no way

300
00:14:24.660 --> 00:14:27.340
I am going to read this. There are a couple

301
00:14:27.340 --> 00:14:30.180
pages of math equations on it, and I would

302
00:14:30.180 --> 00:14:33.180
put you guys to some sleep if I read all of these numbers in a

303
00:14:33.180 --> 00:14:35.980
row, But I am going to paraphrase. So our next

304
00:14:35.980 --> 00:14:38.500
Question is from. I hope I'm saying your name

305
00:14:38.500 --> 00:14:41.380
correctly. East Hawk. And um, I looked it

306
00:14:41.380 --> 00:14:44.380
up. It looks like that's a Slovenian name. So I'm wondering if

307
00:14:44.380 --> 00:14:47.140
you are from Slovenia or not. I love

308
00:14:47.219 --> 00:14:49.860
Slovenia. Beautiful, beautiful country. But

309
00:14:49.980 --> 00:14:52.820
um, East Hawk says the other day. Do you

310
00:14:53.620 --> 00:14:56.460
see if I can even read the question if I paraphrase

311
00:14:56.460 --> 00:14:59.420
it? The other day you discussed the density

312
00:14:59.420 --> 00:15:02.110
of black holes. And then he goes on

313
00:15:02.110 --> 00:15:04.910
to um, say that he looked up an AI

314
00:15:04.910 --> 00:15:07.670
formula, um, to compare the density of a

315
00:15:07.670 --> 00:15:10.150
proton with the density of a black hole.

316
00:15:10.470 --> 00:15:13.030
And he's trying to calculate the density

317
00:15:13.190 --> 00:15:15.910
using um, for each, using a

318
00:15:15.910 --> 00:15:18.870
formula. And then he goes on and on and

319
00:15:18.870 --> 00:15:21.430
on, um, with. With these

320
00:15:21.510 --> 00:15:24.230
formulas. And then for a black hole, we'll consider

321
00:15:24.790 --> 00:15:27.350
a Schwarzschild black hole, which is the

322
00:15:27.350 --> 00:15:30.190
simplest type of black hole. The density of a black hole

323
00:15:30.190 --> 00:15:33.020
depends on its mass. Let's take this example

324
00:15:33.420 --> 00:15:35.980
more equations. And key is

325
00:15:35.980 --> 00:15:38.140
basically just asking if,

326
00:15:38.250 --> 00:15:41.180
um, the density of a black hole is

327
00:15:41.180 --> 00:15:44.020
significantly higher than that of a proton. This

328
00:15:44.020 --> 00:15:46.060
comparison illustrates the extreme

329
00:15:46.140 --> 00:15:48.620
compactness of black holes

330
00:15:49.100 --> 00:15:52.020
where a large mass is compressed into a very

331
00:15:52.020 --> 00:15:54.940
small volume, leading to incredibly high

332
00:15:55.580 --> 00:15:58.190
densities. Fred, you've got this

333
00:15:58.190 --> 00:16:01.110
math um, thesis in front of you, so

334
00:16:01.110 --> 00:16:03.950
you, you can break it down

335
00:16:03.950 --> 00:16:04.470
for us.

336
00:16:05.190 --> 00:16:07.990
Professor Fred Watson: No, you've, you've summarized it perfectly, Heidi. And

337
00:16:08.150 --> 00:16:10.550
so. Yes, so what, what we do is look at,

338
00:16:11.270 --> 00:16:13.750
so density is mass over volume.

339
00:16:14.190 --> 00:16:17.190
Uh, and uh, that's a simple calculation. And we

340
00:16:17.190 --> 00:16:20.190
can do it, I mean, you know, in school physics you

341
00:16:20.190 --> 00:16:22.970
do it for, for lumps of wood or

342
00:16:22.970 --> 00:16:25.890
things like that to work out what the volume is and what the mass

343
00:16:25.890 --> 00:16:28.850
is. And then you get the density. Uh, it's

344
00:16:28.850 --> 00:16:31.690
a little bit different when you're looking at subatomic particles like

345
00:16:31.690 --> 00:16:34.170
a proton. Uh, but you can do the

346
00:16:34.410 --> 00:16:36.650
same sort of calculations.

347
00:16:37.050 --> 00:16:39.930
And um. Yes. So the AI,

348
00:16:40.430 --> 00:16:43.210
uh, that is toc, uh, relied

349
00:16:43.210 --> 00:16:45.730
on. I uh, think got the density of a

350
00:16:45.730 --> 00:16:48.730
proton approximately correct. Uh, at

351
00:16:48.730 --> 00:16:51.290
6.73 times 10 to the power 17

352
00:16:51.610 --> 00:16:54.550
kilograms per cubic meter. Um,

353
00:16:54.630 --> 00:16:57.150
it's very dense, a proton. But then the

354
00:16:57.150 --> 00:16:59.910
calculation goes on to uh, estimate the

355
00:16:59.910 --> 00:17:02.390
density of a black hole. Um, and

356
00:17:02.550 --> 00:17:04.550
actually comes out with the not surprising

357
00:17:05.930 --> 00:17:08.910
uh, result, um, that the black hole is more dense than

358
00:17:08.910 --> 00:17:11.910
the proton. Uh, about, uh.

359
00:17:12.070 --> 00:17:15.070
With a, with a ratio of, um. I think

360
00:17:15.070 --> 00:17:17.430
it's more than 100. Actually more than 100 times.

361
00:17:18.310 --> 00:17:20.820
Um. The only thing is, I think that the

362
00:17:20.820 --> 00:17:23.820
AI might have misled you. There is tak.

363
00:17:23.820 --> 00:17:26.820
Because what the AI has done is taken,

364
00:17:26.900 --> 00:17:29.220
as Heidi mentioned, it's the uh,

365
00:17:29.220 --> 00:17:32.140
Schwarzschild radius, uh, which is the

366
00:17:32.140 --> 00:17:35.100
radius of the event horizon. Um, and

367
00:17:35.100 --> 00:17:37.860
that's not the radius of the black hole.

368
00:17:37.940 --> 00:17:40.820
AI might think it is. Uh, but it's not,

369
00:17:41.140 --> 00:17:43.820
because the radius of a black hole is

370
00:17:43.820 --> 00:17:46.500
zero by definition, and that means

371
00:17:46.580 --> 00:17:49.480
its density, because mass over volume,

372
00:17:49.810 --> 00:17:52.440
uh, it's the mass which does have a parameter

373
00:17:52.680 --> 00:17:55.560
over the volume, which is effectively zero, that gives

374
00:17:55.560 --> 00:17:58.560
you basically an infinite density. And that's

375
00:17:58.560 --> 00:18:01.160
one definition of a black hole is a point in space

376
00:18:02.520 --> 00:18:05.130
where the density is infinite. Um,

377
00:18:05.240 --> 00:18:07.840
now we don't know whether real black

378
00:18:07.840 --> 00:18:10.520
holes have infinite density, but they are

379
00:18:10.520 --> 00:18:12.920
probably, um, you know,

380
00:18:13.480 --> 00:18:14.890
enough of, uh,

381
00:18:15.620 --> 00:18:17.530
uh, significantly,

382
00:18:18.080 --> 00:18:20.690
um, significantly more

383
00:18:20.690 --> 00:18:23.490
dense than any of the densities that we

384
00:18:23.490 --> 00:18:26.210
might calculate for, for example, subatomic

385
00:18:26.210 --> 00:18:29.170
particles like protons. Um, so, um, I

386
00:18:29.170 --> 00:18:31.930
think the AI might have made a slight error there,

387
00:18:32.250 --> 00:18:35.050
but the answer is the same. The density of a black

388
00:18:35.050 --> 00:18:38.010
hole is very, very high indeed and may be

389
00:18:38.010 --> 00:18:40.890
infinite. Um, so a really interesting piece of,

390
00:18:41.060 --> 00:18:43.950
um, research by you. He's talk. Well done

391
00:18:43.950 --> 00:18:46.870
on doing that. Uh, and, um, thank you for

392
00:18:46.870 --> 00:18:49.750
sending it to us to see your calculations. It's nice to

393
00:18:49.750 --> 00:18:52.750
see some mathematics appearing in our

394
00:18:52.750 --> 00:18:53.320
questions there.

395
00:18:53.320 --> 00:18:56.190
Heidi Campo: Uh, yeah, uh, quite a few

396
00:18:56.190 --> 00:18:57.470
mathematics. It was very fun.

397
00:19:00.430 --> 00:19:02.670
Andrew Dunkley: Three, two, one.

398
00:19:03.310 --> 00:19:03.710
Space.

399
00:19:03.870 --> 00:19:04.510
Heidi Campo: Nuts.

400
00:19:05.020 --> 00:19:07.670
Um, our last question of the day is an audio

401
00:19:07.670 --> 00:19:10.590
question. And I don't think you mentioned your name in this

402
00:19:10.590 --> 00:19:13.550
question, but this is another great

403
00:19:13.630 --> 00:19:16.590
question that we are going to let Fred cue

404
00:19:16.590 --> 00:19:19.150
up and listen to and we're going to play this question for

405
00:19:19.630 --> 00:19:20.070
all y'.

406
00:19:20.070 --> 00:19:22.830
Professor Fred Watson: All. Now, space is huge and getting

407
00:19:23.310 --> 00:19:26.190
much, much bigger. Is

408
00:19:26.190 --> 00:19:29.030
it possible that at the beginning of the Big

409
00:19:29.030 --> 00:19:31.390
Bang or soon after the

410
00:19:31.390 --> 00:19:33.310
microbes were made up, uh, life

411
00:19:34.990 --> 00:19:37.920
was generated and therefore this

412
00:19:37.920 --> 00:19:40.560
was spread across the universe

413
00:19:41.440 --> 00:19:43.840
over time. Thank you.

414
00:19:44.560 --> 00:19:45.600
Heidi Campo: I do love the birds.

415
00:19:45.760 --> 00:19:48.640
Professor Fred Watson: Yeah, the birds are wonderful. I, I think that's, um, that's an

416
00:19:48.640 --> 00:19:51.440
Australian accent, I think, and I think they're Australian

417
00:19:51.440 --> 00:19:54.440
birds in the background. Um,

418
00:19:54.440 --> 00:19:57.400
so, um, I'm sorry that we don't know who that was from, but thank

419
00:19:57.400 --> 00:20:00.360
you very much for the question. Uh, and it's, it,

420
00:20:00.360 --> 00:20:03.200
it's interesting. I mean, we, you know, one

421
00:20:03.200 --> 00:20:05.770
of the ideas that were

422
00:20:05.770 --> 00:20:08.650
certainly kind of popular in

423
00:20:08.650 --> 00:20:11.570
the, towards the end of the last century,

424
00:20:11.740 --> 00:20:13.984
um, in the 1970s, 80s,

425
00:20:14.142 --> 00:20:16.930
90s, uh, was that,

426
00:20:17.380 --> 00:20:20.050
uh, it was what we call the panspermia hypothesis,

427
00:20:20.560 --> 00:20:23.490
uh, that life is

428
00:20:23.490 --> 00:20:25.250
common in space and

429
00:20:26.610 --> 00:20:29.450
gets to planets like our own by coming

430
00:20:29.450 --> 00:20:32.360
from space, uh, either, you know,

431
00:20:32.360 --> 00:20:35.120
hitching a ride, some microbes either hitching a ride on,

432
00:20:35.120 --> 00:20:37.960
uh, a meteorite or something. Of

433
00:20:37.960 --> 00:20:40.960
that sort that lands on the Earth, uh, and,

434
00:20:40.980 --> 00:20:43.960
um, that micro or even actually just filtering

435
00:20:43.960 --> 00:20:46.880
down through the atmosphere. Um, there was one of the great

436
00:20:46.880 --> 00:20:49.680
names in British astronomy, in fact,

437
00:20:49.680 --> 00:20:52.160
global astronomy Professor Sir Fred Hoyle.

438
00:20:52.500 --> 00:20:55.420
Uh, he was, um, a very, um,

439
00:20:55.680 --> 00:20:58.600
very gifted scientist who made his mark in the years following

440
00:20:58.600 --> 00:21:01.370
the Second World War. But towards the end of his life,

441
00:21:01.610 --> 00:21:04.500
he espoused this idea of panspermia that, um,

442
00:21:05.130 --> 00:21:07.930
you know, basically living organisms drift through

443
00:21:07.930 --> 00:21:10.850
space and wind up on, um, planets because

444
00:21:10.850 --> 00:21:13.650
of that. Uh, but it's very, it's a very

445
00:21:13.650 --> 00:21:16.570
unpopular idea because of

446
00:21:16.570 --> 00:21:18.970
the physics that are involved.

447
00:21:21.610 --> 00:21:23.770
So what you need is, uh, the raw

448
00:21:24.010 --> 00:21:26.810
materials for life to come together

449
00:21:27.880 --> 00:21:30.800
in the vacuum of space. Well, space is

450
00:21:30.800 --> 00:21:33.320
not a vacuum. We know in interstellar clouds there are significant

451
00:21:33.480 --> 00:21:36.480
numbers of chemicals. Uh, and in fact, we do know that

452
00:21:36.480 --> 00:21:39.440
the building blocks of life, such as amino acids and things of

453
00:21:39.440 --> 00:21:41.880
that sort, are actually present in some of these

454
00:21:41.880 --> 00:21:44.200
clouds of gas and dust.

455
00:21:44.680 --> 00:21:47.480
But, um, for the process of

456
00:21:47.720 --> 00:21:50.680
chemistry to give rise to the processes of

457
00:21:50.680 --> 00:21:53.610
biology, uh, you need conditions which

458
00:21:53.610 --> 00:21:56.050
we think only occur on planets where

459
00:21:56.210 --> 00:21:57.970
there's gravitational binding.

460
00:21:58.780 --> 00:22:01.730
Um, you need to form membranes

461
00:22:01.730 --> 00:22:04.610
to basically be the walls of cells. So that

462
00:22:04.610 --> 00:22:07.170
when you produce a single celled living organism,

463
00:22:08.210 --> 00:22:10.770
it's not just a bunch of atoms that leak out into its

464
00:22:10.770 --> 00:22:13.730
surroundings. It's actually held there. So you need lipids and things of

465
00:22:13.730 --> 00:22:15.890
that sort. Quite complex procedures.

466
00:22:16.690 --> 00:22:19.480
Now, um, in a sense, though, our, uh,

467
00:22:19.480 --> 00:22:22.440
anonymous questioner is right. Because in the aftermath

468
00:22:22.440 --> 00:22:25.320
of the Big Bang, microbes were

469
00:22:25.320 --> 00:22:27.960
certainly not around then because the

470
00:22:27.960 --> 00:22:29.920
conditions, you know, temperature and

471
00:22:30.480 --> 00:22:33.320
pressures, uh, were far too

472
00:22:33.320 --> 00:22:36.160
high for any molecules at all to exist.

473
00:22:36.160 --> 00:22:39.040
Molecules would have been shredded apart, uh, let

474
00:22:39.040 --> 00:22:42.000
alone living organisms. So microbes did not,

475
00:22:42.200 --> 00:22:45.110
uh, come out about as, as part of the Big

476
00:22:45.110 --> 00:22:47.910
Bang, but the raw materials

477
00:22:47.910 --> 00:22:50.550
did, uh, the hydrogen and helium, which

478
00:22:50.710 --> 00:22:53.590
were created in the Big Bang, uh, that was spread

479
00:22:53.590 --> 00:22:56.470
throughout the universe. And what happened

480
00:22:56.470 --> 00:22:58.910
next was, um, the formation of

481
00:22:58.910 --> 00:23:01.870
stars, uh, by hydrogen clouds

482
00:23:01.870 --> 00:23:04.150
collapsing under their own weight and switching on,

483
00:23:04.860 --> 00:23:07.590
um, the processes that generate

484
00:23:08.870 --> 00:23:11.590
the nuclear fusion that actually causes star to shine.

485
00:23:11.830 --> 00:23:14.590
Not only do they generate energy, which we're

486
00:23:14.590 --> 00:23:17.330
feeling right now from the, uh, they

487
00:23:17.330 --> 00:23:20.250
also create new elements. And it's

488
00:23:20.250 --> 00:23:23.130
those new elements, the oxygen, the carbon, the hydrogen, the

489
00:23:23.130 --> 00:23:25.690
nitrogen, all of those things are the raw

490
00:23:25.690 --> 00:23:28.530
materials of life. Uh, and so the raw

491
00:23:28.530 --> 00:23:31.510
materials of microbes were produced, uh,

492
00:23:31.510 --> 00:23:34.490
not initially in the Big Bang, but everything was there that

493
00:23:34.490 --> 00:23:37.490
we needed later on. And so it is possible

494
00:23:38.210 --> 00:23:41.090
that if you have microbial life, and it may only occur

495
00:23:41.090 --> 00:23:43.810
on planets, but planets Are everywhere in the universe.

496
00:23:44.250 --> 00:23:47.140
Uh, the raw ingredients are there everywhere in

497
00:23:47.140 --> 00:23:50.140
the universe. And so, yes, maybe there are microbes everywhere

498
00:23:50.140 --> 00:23:53.100
in the universe. Whether they come to us from space, that's a different

499
00:23:53.100 --> 00:23:56.100
matter. But, uh, certainly

500
00:23:56.980 --> 00:23:59.620
in the sense that our questioner, ah, ah, has asked,

501
00:23:59.800 --> 00:24:02.400
um, it's everywhere. Um,

502
00:24:03.540 --> 00:24:05.940
because the raw materials were spread throughout the universe,

503
00:24:06.260 --> 00:24:09.220
life could probably exist anywhere in

504
00:24:09.220 --> 00:24:12.060
the universe. The only issue is we haven't found it yet. And

505
00:24:12.060 --> 00:24:14.930
that's the rather annoying part of this whole issue. Whole matter.

506
00:24:15.650 --> 00:24:18.290
So, um, let's keep working on that. Uh, looking

507
00:24:18.290 --> 00:24:20.930
for first signs of life beyond Earth.

508
00:24:22.450 --> 00:24:25.330
Heidi Campo: Yeah, if you guys, if you guys are hooked on math still,

509
00:24:25.330 --> 00:24:27.940
you can look up the Drake equation. That's a fun little, uh,

510
00:24:28.170 --> 00:24:30.970
deep dive you can go on to. But I just love that this

511
00:24:30.970 --> 00:24:33.810
question was about life in the background of it.

512
00:24:33.810 --> 00:24:36.800
I'm still fixated on the birds for whatever reason. It sounded like,

513
00:24:36.800 --> 00:24:39.650
um, he was coming from some kind of like

514
00:24:39.650 --> 00:24:42.490
conservatory or a jungle. And it was just so, so

515
00:24:42.490 --> 00:24:45.250
rich in life. Like, I feel like I was in some kind of like a greenhouse

516
00:24:45.250 --> 00:24:48.140
with like, you know, bugs and butterflies and insects

517
00:24:48.140 --> 00:24:51.060
and birds all around me. It's very cool. And you know what, at

518
00:24:51.060 --> 00:24:53.820
the end of the day, this planet rocks. I really,

519
00:24:53.900 --> 00:24:55.260
really like our planet.

520
00:24:56.620 --> 00:24:59.540
Space is fantastic, but when

521
00:24:59.540 --> 00:25:02.500
you, when you really kind of, you, you take

522
00:25:02.500 --> 00:25:05.500
your eyes away from the stars and you look at what we've got going on here, it's like,

523
00:25:05.500 --> 00:25:08.380
wow, this is, this is pretty nice. We've got a

524
00:25:08.380 --> 00:25:11.260
really good looking planet here. And it

525
00:25:11.260 --> 00:25:13.740
really is incredible to think it's like everything

526
00:25:13.900 --> 00:25:16.460
that's out there. There's no planet like Earth.

527
00:25:16.840 --> 00:25:19.560
We really are on such a beautiful, special

528
00:25:19.560 --> 00:25:20.120
planet.

529
00:25:21.320 --> 00:25:24.160
Professor Fred Watson: We are. And that's a very important point because

530
00:25:24.160 --> 00:25:27.120
most of us simply take it for granted and don't

531
00:25:27.120 --> 00:25:29.760
really think about life beyond Earth or, uh,

532
00:25:30.600 --> 00:25:33.240
space. I mean, you know, when you ask people

533
00:25:33.400 --> 00:25:36.240
in the street, uh, they don't

534
00:25:36.240 --> 00:25:39.080
realize that the Earth could be unique, is

535
00:25:39.240 --> 00:25:42.120
so, so precious because it's actually got

536
00:25:42.120 --> 00:25:44.920
exactly the right ingredients for the kind of life forms that we

537
00:25:44.920 --> 00:25:47.580
are. And we've evolved from that. We're

538
00:25:47.730 --> 00:25:48.690
product of our environment.

539
00:25:50.210 --> 00:25:52.970
Heidi Campo: Yeah, yeah. And then we produce, you know, all

540
00:25:52.970 --> 00:25:55.490
sorts of things with this gift of life, including

541
00:25:55.730 --> 00:25:56.690
podcasts.

542
00:25:58.610 --> 00:26:01.570
It's just the human ingenuity never, never stops.

543
00:26:02.200 --> 00:26:04.850
Um, but yeah, that is, that is it for the

544
00:26:04.850 --> 00:26:07.810
questions for today's episode. Guys, you're fantastic.

545
00:26:07.890 --> 00:26:10.770
Please keep sending in your amazing questions. I

546
00:26:10.770 --> 00:26:13.490
love to hear them. Fred loves to answer them.

547
00:26:13.730 --> 00:26:14.130
And.

548
00:26:14.370 --> 00:26:14.930
Professor Fred Watson: Oh, m. No.

549
00:26:16.830 --> 00:26:18.830
Heidi Campo: And it's always. It's always such a pleasure.

550
00:26:20.110 --> 00:26:22.910
Professor Fred Watson: And as it is for me. You're quite right, Heidi. I love getting

551
00:26:22.910 --> 00:26:25.590
these questions. They. They challenge my brain, which

552
00:26:25.590 --> 00:26:27.630
is, um, a good thing to have.

553
00:26:29.550 --> 00:26:32.310
Heidi Campo: Yeah, well, I'm sure you're going to have a lot of questions. Fred

554
00:26:32.310 --> 00:26:35.310
is. It's a. It's a Sunday night for me, so I'm winding

555
00:26:35.310 --> 00:26:38.310
down. I think my husband's making, um, tuna steaks

556
00:26:38.310 --> 00:26:41.230
tonight, and then Fred is ramping up on a Monday morning.

557
00:26:41.850 --> 00:26:44.810
Heading off to your conferences. I can't wait to hear how

558
00:26:44.810 --> 00:26:47.730
these go. They sound like it's going to be a very fun, fun time

559
00:26:47.730 --> 00:26:48.170
for you.

560
00:26:49.050 --> 00:26:52.010
Professor Fred Watson: I'll, uh, I'll be sure to fill you in on everything that goes on.

561
00:26:52.010 --> 00:26:54.810
Thanks. Good to talk and speak again soon.

562
00:26:55.050 --> 00:26:56.360
Heidi Campo: All right. Take care, Fred. Bye bye.

563
00:26:56.360 --> 00:26:59.160
Voice Over Guy: You've been listening to the SpaceNuts podcast,

564
00:27:00.680 --> 00:27:03.480
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566
00:27:06.410 --> 00:27:09.410
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567
00:27:09.360 --> 00:27:12.020
Um, this has been another quality podcast

568
00:27:12.020 --> 00:27:13.620
production from bitesz.com