1 00:00:08,680 --> 00:00:11,800 Speaker 1: Hey, Daniel, what's the biggest number you can hold in 2 00:00:11,840 --> 00:00:15,880 Speaker 1: your head? I can think about infinity, I guess, can 3 00:00:15,960 --> 00:00:19,439 Speaker 1: you do have an infinite number of neurons? No, but 4 00:00:19,600 --> 00:00:22,000 Speaker 1: it feels like I've eaten an infinite number of cookies 5 00:00:22,120 --> 00:00:25,680 Speaker 1: during this pandemic. It does feel like it's dragging onto infinity. 6 00:00:27,200 --> 00:00:29,080 Speaker 1: But you know, even if you ate a hundred cookies 7 00:00:29,120 --> 00:00:31,440 Speaker 1: a day, that's not even a million cookies a year. 8 00:00:31,520 --> 00:00:35,599 Speaker 1: Although that's a good goal to happen, you're right, And honestly, 9 00:00:35,760 --> 00:00:38,800 Speaker 1: it's hard to visualize a number bigger than like a 10 00:00:38,920 --> 00:00:41,960 Speaker 1: hundred or a thousand anything else. In my head. Frankly, 11 00:00:42,000 --> 00:00:46,680 Speaker 1: it's just like a lot, a bunch, a zillion. So 12 00:00:46,680 --> 00:00:48,440 Speaker 1: then how do you think about how big things are 13 00:00:48,479 --> 00:00:52,000 Speaker 1: out in space, like Jupiter or the Sun or the galaxy? Like, 14 00:00:52,040 --> 00:00:54,640 Speaker 1: how do you conceive or think about the mass of 15 00:00:54,720 --> 00:00:57,840 Speaker 1: such huge objects? I just use the unit of cookies. 16 00:00:58,040 --> 00:01:00,600 Speaker 1: Jupiter is a whole lot of cookies. It's a pandemic 17 00:01:00,600 --> 00:01:03,280 Speaker 1: bard fool of cookies. It's the biggest cookie jar in 18 00:01:03,320 --> 00:01:05,640 Speaker 1: the universe. That's my goal in this pandemic. To eat 19 00:01:05,720 --> 00:01:08,560 Speaker 1: one Jupiter's worth of cookies. Then you look like Jupiter 20 00:01:10,520 --> 00:01:12,959 Speaker 1: I think we just wrote Jupiter's formation story for the 21 00:01:13,000 --> 00:01:30,640 Speaker 1: comic book series. I am more hammade cartoonists and the 22 00:01:30,680 --> 00:01:34,800 Speaker 1: creator of PhD comments. Hi. I'm Daniel. I'm a particle physicist, 23 00:01:34,840 --> 00:01:38,280 Speaker 1: but I have strong opinions about cookies. Do you really 24 00:01:38,640 --> 00:01:41,880 Speaker 1: like a positive or negative like you're never ambivalent about cookies. 25 00:01:42,040 --> 00:01:45,200 Speaker 1: I'm never ambivalent about cookies and very specific taste for 26 00:01:45,360 --> 00:01:48,680 Speaker 1: what makes a good cookie really according to you? Or 27 00:01:48,720 --> 00:01:51,240 Speaker 1: do you think you have some sort of universal standard 28 00:01:51,320 --> 00:01:54,560 Speaker 1: of cookie goodness. I would not want to be the 29 00:01:54,560 --> 00:01:59,320 Speaker 1: cookie spokesperson for humanity, but I have strong reactions to cookies. Yes, really, 30 00:01:59,360 --> 00:02:01,240 Speaker 1: What do you think about hips of hoyies? Those are 31 00:02:01,240 --> 00:02:09,480 Speaker 1: not cookies, My god, those are cardboards simulcrums of cookies. Man, Well, 32 00:02:09,480 --> 00:02:12,560 Speaker 1: welcome to our podcast. Daniel and Jorge explain the universe 33 00:02:12,720 --> 00:02:16,840 Speaker 1: of cookies, just the regular universe, the other universe, A 34 00:02:17,000 --> 00:02:19,639 Speaker 1: production of I Heart Radio, in which we take our 35 00:02:19,800 --> 00:02:23,760 Speaker 1: cookie fueled brains on a tour of everything in the universe, 36 00:02:23,800 --> 00:02:26,440 Speaker 1: how it works, how big it is, how small it is. 37 00:02:26,760 --> 00:02:30,480 Speaker 1: Nothing on this podcast is too vast, too incredibly huge 38 00:02:30,520 --> 00:02:33,400 Speaker 1: for us to try to wrap our minds around. Nor 39 00:02:33,520 --> 00:02:36,200 Speaker 1: is it too small for us to try to penetrate 40 00:02:36,240 --> 00:02:38,760 Speaker 1: with our intellect and get a grasp of what's going 41 00:02:38,880 --> 00:02:41,720 Speaker 1: on down at the tiniest level. Yeah, because it's pretty 42 00:02:41,720 --> 00:02:44,440 Speaker 1: hard sometimes to hold the hold universe in your head. 43 00:02:44,480 --> 00:02:46,360 Speaker 1: I mean, you have to hold not just the tiny 44 00:02:46,440 --> 00:02:49,120 Speaker 1: microscopic particles that everything is made out of, but you 45 00:02:49,120 --> 00:02:51,880 Speaker 1: also have to hold the ginormous structures that are out 46 00:02:51,880 --> 00:02:56,040 Speaker 1: there in space, those huge suns and stars and galaxies 47 00:02:56,080 --> 00:02:59,480 Speaker 1: and solar systems and clusters of galaxies. It's a big universe. 48 00:02:59,600 --> 00:03:01,920 Speaker 1: It is a big universe, and often we just rely 49 00:03:02,040 --> 00:03:05,160 Speaker 1: on math as like a mental scaffolding to take us 50 00:03:05,200 --> 00:03:08,359 Speaker 1: where our minds have a hard time going. We talk 51 00:03:08,400 --> 00:03:11,239 Speaker 1: about these numbers, but it's good to understand that these 52 00:03:11,280 --> 00:03:13,919 Speaker 1: things are real. When we talk about these objects that 53 00:03:13,919 --> 00:03:17,360 Speaker 1: are out there, they're real. They're out there. There's actually enormous, 54 00:03:17,480 --> 00:03:21,200 Speaker 1: vast burning plasma balls in the sky. This is not 55 00:03:21,240 --> 00:03:24,160 Speaker 1: a joke, This is not just notation. It's reality. Yeah, 56 00:03:24,200 --> 00:03:27,160 Speaker 1: they're giant cookies as well, the size of Jupiter. You know. 57 00:03:27,200 --> 00:03:29,800 Speaker 1: I always say we shouldn't be surprised by anything we 58 00:03:29,840 --> 00:03:33,440 Speaker 1: discover in the universe. But if hubble turns up enormous 59 00:03:33,440 --> 00:03:37,600 Speaker 1: planet sized cookies. I would be surprised and delighted. Depends 60 00:03:37,640 --> 00:03:40,320 Speaker 1: on what's in the cookie, man, and if they're Jupiter 61 00:03:40,400 --> 00:03:44,720 Speaker 1: sized chips of hoys, I'm out well. In today's podcast, 62 00:03:44,720 --> 00:03:48,000 Speaker 1: will be tackling another one of our Extreme Universe series, 63 00:03:48,080 --> 00:03:51,280 Speaker 1: in which we talk about the biggest things in the universe, 64 00:03:51,400 --> 00:03:56,120 Speaker 1: the hottest, the coldest, the emptiest bass in the universe. 65 00:03:56,280 --> 00:03:58,440 Speaker 1: We like to talk about extreme things, Yeah, because the 66 00:03:58,480 --> 00:04:01,280 Speaker 1: extremes tell us what's a limit are. That's what reveals 67 00:04:01,320 --> 00:04:04,000 Speaker 1: what the rules are. When you push the universe to 68 00:04:04,120 --> 00:04:06,600 Speaker 1: the edges of what he can do, you understand why 69 00:04:06,640 --> 00:04:08,680 Speaker 1: you can do something and why it can't. So the 70 00:04:08,680 --> 00:04:11,440 Speaker 1: Extreme Universe series is not just fun because it blows 71 00:04:11,440 --> 00:04:13,960 Speaker 1: your mind, but also it teaches us something about the 72 00:04:13,960 --> 00:04:18,599 Speaker 1: way the universe works. Yeah, it's extremely educational as well. 73 00:04:18,880 --> 00:04:21,719 Speaker 1: So on today's podcast will be tackling one of these 74 00:04:21,800 --> 00:04:24,360 Speaker 1: extreme things in the universe, and we're doing something a 75 00:04:24,400 --> 00:04:27,080 Speaker 1: little different today. That's right. Today we have a guest 76 00:04:27,320 --> 00:04:30,760 Speaker 1: who will be asking the question of the episode for us. Yeah, 77 00:04:30,760 --> 00:04:33,839 Speaker 1: he's kind of a bit of a celebrity online, right, Yeah. Absolutely, 78 00:04:33,839 --> 00:04:36,719 Speaker 1: he's definitely the youngest host of a science podcast that 79 00:04:36,920 --> 00:04:40,400 Speaker 1: I'm aware of. Yeah, so here is our special guest 80 00:04:40,480 --> 00:04:43,760 Speaker 1: to introduce the question. Hello, with my pleasure to welcome 81 00:04:43,760 --> 00:04:48,640 Speaker 1: to the program. Today's special guest question asker Tie Pool. Hi, 82 00:04:48,760 --> 00:04:52,039 Speaker 1: say hello to everyone. Hi, I'm really excited to be here. 83 00:04:52,200 --> 00:04:56,000 Speaker 1: I'm a little bit nervous, but mostly excited. Well, welcome 84 00:04:56,000 --> 00:04:57,920 Speaker 1: to the program. Why don't you tell us a little 85 00:04:57,920 --> 00:05:02,240 Speaker 1: bit about yourself and your podcast? Well, I'm fourteen, just 86 00:05:02,400 --> 00:05:06,360 Speaker 1: started high school. I'm here in Toronto, and I host 87 00:05:06,400 --> 00:05:09,839 Speaker 1: a CBC podcast called tie Asks Why the Journey of 88 00:05:09,880 --> 00:05:14,120 Speaker 1: a kid just asking questions because you know, my curiosity 89 00:05:14,160 --> 00:05:18,000 Speaker 1: got the better of me. You asked so many questions 90 00:05:18,040 --> 00:05:20,760 Speaker 1: that they decided you should host a podcast about it. Yeah, 91 00:05:20,800 --> 00:05:23,919 Speaker 1: pretty much. And what kind of topics does your podcast 92 00:05:24,080 --> 00:05:27,679 Speaker 1: ask about or answer? Well, we have a wide range 93 00:05:27,680 --> 00:05:29,680 Speaker 1: of stuff. You know, it can get kind of silly 94 00:05:29,760 --> 00:05:33,160 Speaker 1: stuff like why do we dance? Or how do songs 95 00:05:33,160 --> 00:05:35,680 Speaker 1: get stuck in your head? But we also deal with 96 00:05:35,760 --> 00:05:39,520 Speaker 1: deeper ones like what is love and what is death? 97 00:05:39,760 --> 00:05:42,239 Speaker 1: And then of course we get to some really crazy 98 00:05:42,279 --> 00:05:45,279 Speaker 1: ones like the end of the universe and a pretty 99 00:05:45,279 --> 00:05:49,880 Speaker 1: topical one about viruses. Awesome, it sounds like a lot 100 00:05:49,920 --> 00:05:52,679 Speaker 1: of fun here on the program. We are definitely big 101 00:05:52,720 --> 00:05:56,840 Speaker 1: fans of curiosity for folks or even down to nine 102 00:05:56,880 --> 00:05:58,839 Speaker 1: years old. And I've listened to a bunch of episodes 103 00:05:58,839 --> 00:06:02,000 Speaker 1: of your podcast. It's a lot of fun. So congrats, thanks, 104 00:06:02,120 --> 00:06:05,040 Speaker 1: I'm really honored. I recently listened to your episode about 105 00:06:05,120 --> 00:06:07,680 Speaker 1: John von Newman, and I think it's really cool because 106 00:06:07,680 --> 00:06:09,600 Speaker 1: he's a really cool guy. He just is in the 107 00:06:09,640 --> 00:06:11,839 Speaker 1: background of a lot of science things, but he did 108 00:06:11,839 --> 00:06:15,120 Speaker 1: a lot. Yeah, he definitely was a curious person. All right, 109 00:06:15,200 --> 00:06:18,200 Speaker 1: So then let's dig into today's episode. We have you 110 00:06:18,200 --> 00:06:21,080 Speaker 1: on to be our guest question asker, So why don't 111 00:06:21,120 --> 00:06:25,200 Speaker 1: you introduce for our listeners what today's episode is about. Well, 112 00:06:25,480 --> 00:06:27,400 Speaker 1: I got another question and I decided to be a 113 00:06:27,440 --> 00:06:29,480 Speaker 1: good idea to ask you guys. So the question for 114 00:06:29,480 --> 00:06:34,680 Speaker 1: this episode is what is the biggest star in the universe? Awesome? 115 00:06:34,880 --> 00:06:37,960 Speaker 1: I love that question. But tell me first, what tickles 116 00:06:37,960 --> 00:06:40,560 Speaker 1: you about that question? What makes you curious about the 117 00:06:40,640 --> 00:06:44,000 Speaker 1: size of stars? Well, it's just kind of thinking about 118 00:06:44,040 --> 00:06:46,239 Speaker 1: the sun, and it's a strange thing to think about. 119 00:06:46,800 --> 00:06:49,839 Speaker 1: It seems like really big and scale of our planets 120 00:06:49,839 --> 00:06:53,040 Speaker 1: and stuff. But I kind of learned and realized that 121 00:06:53,120 --> 00:06:55,960 Speaker 1: our son is not very big in comparison to other stars. 122 00:06:56,000 --> 00:06:58,560 Speaker 1: So it kind of just got me thinking, like how 123 00:06:58,640 --> 00:07:01,560 Speaker 1: big could we reallyly go? You know, can we get 124 00:07:01,600 --> 00:07:03,640 Speaker 1: something that's like twice the size of our stunt? Is 125 00:07:03,680 --> 00:07:06,240 Speaker 1: that the biggest or like a million times we go 126 00:07:06,360 --> 00:07:09,840 Speaker 1: like really really big? Awesome? Well, I love your expectation 127 00:07:09,960 --> 00:07:12,840 Speaker 1: that the universe will surprise you, will shock you, because 128 00:07:12,880 --> 00:07:15,000 Speaker 1: I think there's a lot of examples in history where 129 00:07:15,000 --> 00:07:17,440 Speaker 1: we learned something about the universe and we are totally 130 00:07:17,440 --> 00:07:20,320 Speaker 1: surprised at the size of things, about the scale of 131 00:07:20,360 --> 00:07:23,880 Speaker 1: the crazy stuff that's going on out there in the universe. Yeah, 132 00:07:24,040 --> 00:07:25,840 Speaker 1: I kind of just was in the mood to get 133 00:07:25,880 --> 00:07:30,320 Speaker 1: my mind blown. You know, I'm excited to hear the number. 134 00:07:30,320 --> 00:07:32,320 Speaker 1: It's gonna be crazy. It's gonna be like a billion 135 00:07:32,400 --> 00:07:36,000 Speaker 1: or something. All right, Well, thanks very much. We'll hope 136 00:07:36,040 --> 00:07:39,440 Speaker 1: to blow your mind. All right. That was Tie Pool, 137 00:07:39,440 --> 00:07:43,280 Speaker 1: host of TI ask why, and like him, I think 138 00:07:43,320 --> 00:07:45,280 Speaker 1: we're all ready to get our mind bloom. That's right. 139 00:07:45,280 --> 00:07:47,520 Speaker 1: It's a lot of pressure though, right, he's really expecting 140 00:07:47,560 --> 00:07:50,600 Speaker 1: a big number. Yeah, yeah, because you know, I bet 141 00:07:50,600 --> 00:07:52,800 Speaker 1: there are huge stars out there in the universe. There 142 00:07:52,840 --> 00:07:55,160 Speaker 1: are huge stars out there in the universe, and Ty 143 00:07:55,360 --> 00:07:57,600 Speaker 1: was reaching for what he thought was like a vast 144 00:07:57,760 --> 00:08:00,320 Speaker 1: number of star, a million times bigger than our son. 145 00:08:00,440 --> 00:08:03,320 Speaker 1: But actually we're going to deliver something much much bigger 146 00:08:03,320 --> 00:08:05,440 Speaker 1: than that, bigger than a million times the size of 147 00:08:05,440 --> 00:08:08,440 Speaker 1: our son. That's right. We're gonna make our son look 148 00:08:08,520 --> 00:08:12,760 Speaker 1: like a tiny dust spec, a shiny, tiny dustpec. Al right, Well, 149 00:08:12,800 --> 00:08:14,880 Speaker 1: as usual, you also went out there into the wilds 150 00:08:14,880 --> 00:08:18,040 Speaker 1: of the Internet to ask regular listeners what they thought 151 00:08:18,040 --> 00:08:20,240 Speaker 1: of this question. That's right, So thank you to everybody 152 00:08:20,240 --> 00:08:23,360 Speaker 1: who stretched their minds and tried to imagine an enormous 153 00:08:23,480 --> 00:08:25,600 Speaker 1: star out there in the universe. And if you would 154 00:08:25,640 --> 00:08:28,880 Speaker 1: like to respond to tough questions from a physicist without 155 00:08:28,920 --> 00:08:32,280 Speaker 1: any reference materials, please write to me two questions at 156 00:08:32,360 --> 00:08:34,600 Speaker 1: Daniel and Jorge dot com. So think about it for 157 00:08:34,600 --> 00:08:37,400 Speaker 1: a second. If someone asked you what you thought was 158 00:08:37,480 --> 00:08:40,679 Speaker 1: the biggest star in the universe, what would you say. 159 00:08:41,080 --> 00:08:44,120 Speaker 1: Here's what people had to say. I think that a 160 00:08:44,200 --> 00:08:48,120 Speaker 1: big factor for determining how big a star can get. 161 00:08:48,640 --> 00:08:52,600 Speaker 1: I think it's gravity. Well, one thing for sure, it's 162 00:08:52,760 --> 00:08:58,800 Speaker 1: they always discovered something that is bigger than they thought 163 00:08:58,840 --> 00:09:02,800 Speaker 1: it would be. That stars can get much more massive 164 00:09:02,880 --> 00:09:05,360 Speaker 1: than our own son. I do not know how big 165 00:09:05,360 --> 00:09:07,720 Speaker 1: a star can get, but I know that at a 166 00:09:07,720 --> 00:09:11,480 Speaker 1: certain point it, when it passes a certain threshold, it 167 00:09:11,559 --> 00:09:15,680 Speaker 1: will collapse on itself and from a black hole. All right, Well, 168 00:09:15,840 --> 00:09:18,640 Speaker 1: the answer seemed to be all over the place, big 169 00:09:18,679 --> 00:09:22,640 Speaker 1: answers and small answers. Yeah, exactly, definitely. People are prepared 170 00:09:22,720 --> 00:09:25,480 Speaker 1: to have their minds blown and to be surprised. I 171 00:09:25,520 --> 00:09:27,720 Speaker 1: think one thing we've learned in our exploration of the 172 00:09:27,800 --> 00:09:31,160 Speaker 1: universe is that what we expect is very rarely what's 173 00:09:31,240 --> 00:09:35,360 Speaker 1: actually out there. Yeah. Well, I think maybe to start 174 00:09:35,559 --> 00:09:39,400 Speaker 1: us off, maybe we should settle this technical question, which 175 00:09:39,440 --> 00:09:41,720 Speaker 1: is I think is important. What do we mean by 176 00:09:41,720 --> 00:09:44,680 Speaker 1: biggest star? Do we mean the biggest in volume, like 177 00:09:44,800 --> 00:09:48,040 Speaker 1: the one that occupies the most space, or the dancest 178 00:09:48,360 --> 00:09:51,280 Speaker 1: or most massive star. What are we talking about here? 179 00:09:51,520 --> 00:09:55,160 Speaker 1: Most paparazzi following them around taking pictures? Maybe, yeah, most 180 00:09:55,240 --> 00:09:59,760 Speaker 1: Instagram followers, biggest box office. That's right, that's what it 181 00:09:59,800 --> 00:10:02,600 Speaker 1: take to be massive on social media. Though it's a 182 00:10:02,640 --> 00:10:05,360 Speaker 1: fair question that you can make an argument in either direction. 183 00:10:05,720 --> 00:10:08,320 Speaker 1: Mass is really important in determining the life cycle of 184 00:10:08,320 --> 00:10:11,160 Speaker 1: a star, and what it means. But volume is also 185 00:10:11,240 --> 00:10:13,640 Speaker 1: a big deal. Really in the end, maybe what we're 186 00:10:13,640 --> 00:10:16,839 Speaker 1: talking about is like the physical size of these things. Yeah, 187 00:10:16,840 --> 00:10:18,320 Speaker 1: because when you see it, when you're in front of 188 00:10:18,320 --> 00:10:19,840 Speaker 1: it at this point, you would think about when you 189 00:10:19,880 --> 00:10:22,319 Speaker 1: think about the word big, like, oh, wow, that's big. 190 00:10:22,360 --> 00:10:24,120 Speaker 1: But if it was small and dense, you've been impressed, 191 00:10:24,160 --> 00:10:26,719 Speaker 1: but you wouldn't say, wow, that's big. Yeah. Well it's 192 00:10:26,720 --> 00:10:29,160 Speaker 1: a big deal, right. It makes a big dent in 193 00:10:29,200 --> 00:10:32,840 Speaker 1: the structure of the universe. It's like a large gravitational well, 194 00:10:33,000 --> 00:10:34,880 Speaker 1: I mean, black holes are not a tiny thing to 195 00:10:34,920 --> 00:10:38,880 Speaker 1: be ignored. And I think initially I would have voted 196 00:10:38,920 --> 00:10:41,440 Speaker 1: for the mass of the star because that really does 197 00:10:41,559 --> 00:10:43,960 Speaker 1: tell you about the nature of the star and also 198 00:10:44,080 --> 00:10:46,640 Speaker 1: like its fate. The entire fate of the star is 199 00:10:46,679 --> 00:10:49,560 Speaker 1: determined by how much stuff it has. If it has 200 00:10:49,559 --> 00:10:51,080 Speaker 1: a certain amount of stuff, it's going to end up 201 00:10:51,080 --> 00:10:52,920 Speaker 1: as a white dwarf that has more, it's gonna become 202 00:10:52,920 --> 00:10:55,120 Speaker 1: a neutron star or eventually a black hole. All of 203 00:10:55,160 --> 00:10:57,760 Speaker 1: that is determined by the mass of the star. It's 204 00:10:57,760 --> 00:11:01,360 Speaker 1: a really important way to categorize stars. And I guess 205 00:11:01,360 --> 00:11:04,400 Speaker 1: it doesn't change because the volume of a star changes, right, 206 00:11:04,440 --> 00:11:07,400 Speaker 1: Like stars go through a life cycle and they grow 207 00:11:07,480 --> 00:11:10,160 Speaker 1: and they shrank and they end up small at the end. Right, 208 00:11:10,760 --> 00:11:13,559 Speaker 1: it's a varying quantity. But the math doesn't really change, 209 00:11:13,600 --> 00:11:15,800 Speaker 1: does it. It doesn't change that much. I mean, the 210 00:11:15,960 --> 00:11:18,040 Speaker 1: end cycle of a star, it does blow off some 211 00:11:18,080 --> 00:11:20,439 Speaker 1: of its outer layers. So, for example, our sun is 212 00:11:20,440 --> 00:11:21,960 Speaker 1: going to end up as a white dwarf, and it 213 00:11:22,000 --> 00:11:24,120 Speaker 1: won't have all the mass that it had in it's 214 00:11:24,160 --> 00:11:26,000 Speaker 1: early part of its life because it's going to blow 215 00:11:26,040 --> 00:11:28,720 Speaker 1: out a huge amount of that into like a planetary nebula. 216 00:11:28,840 --> 00:11:30,640 Speaker 1: So it does sort of change. But you know, you 217 00:11:30,720 --> 00:11:33,400 Speaker 1: might say that by the time our sun becomes a 218 00:11:33,400 --> 00:11:35,880 Speaker 1: white dwarf, it's no longer a star, right because it 219 00:11:35,880 --> 00:11:38,760 Speaker 1: has no more fusion going on inside of it. To 220 00:11:38,880 --> 00:11:43,480 Speaker 1: see list celebrity now exactly can't even get into the 221 00:11:43,520 --> 00:11:46,160 Speaker 1: hottest restaurants in l A anymore. It's in dancing with 222 00:11:46,240 --> 00:11:51,960 Speaker 1: the stars, exactly. But volume, you're right, it's variable. Star 223 00:11:52,040 --> 00:11:54,200 Speaker 1: can grow a lot during its life cycle. So if 224 00:11:54,200 --> 00:11:57,000 Speaker 1: we just look out into space and compare two stars, 225 00:11:57,040 --> 00:11:59,560 Speaker 1: we might be comparing two stars that eventually would have 226 00:11:59,640 --> 00:12:01,360 Speaker 1: the same size. If you sort of lined them up. 227 00:12:01,400 --> 00:12:03,400 Speaker 1: But one of them is like a grandpa star that's 228 00:12:03,400 --> 00:12:05,040 Speaker 1: really big at the end of his life. The other 229 00:12:05,040 --> 00:12:07,880 Speaker 1: one it's like a baby star that's more condensed. Okay, 230 00:12:07,880 --> 00:12:10,480 Speaker 1: so then we're really talking about the mass of the 231 00:12:10,480 --> 00:12:13,400 Speaker 1: star then, like what's the most massive star? Yeah, I 232 00:12:13,440 --> 00:12:15,920 Speaker 1: don't know. I'm honestly on the fence about it, because 233 00:12:16,120 --> 00:12:18,440 Speaker 1: the mass of the star is also important for other reasons, 234 00:12:18,480 --> 00:12:20,640 Speaker 1: Like it tells you about the history of the universe. 235 00:12:20,679 --> 00:12:23,360 Speaker 1: You know, the very early universe stars were much bigger 236 00:12:23,360 --> 00:12:26,800 Speaker 1: and hotter and burned faster because there weren't these pockets 237 00:12:26,800 --> 00:12:29,720 Speaker 1: of metal to collapse smaller stars, and later on the 238 00:12:29,760 --> 00:12:33,200 Speaker 1: stars that were formed are smaller and lasts longer, So 239 00:12:33,400 --> 00:12:36,040 Speaker 1: that's really important. On the other hand, what I think 240 00:12:36,080 --> 00:12:38,840 Speaker 1: about what is the biggest star in the universe, I 241 00:12:38,880 --> 00:12:41,440 Speaker 1: definitely am thinking about volume. I want my mind blown 242 00:12:41,440 --> 00:12:45,360 Speaker 1: by the sheer amount of space that this thing takes up. Right, 243 00:12:45,440 --> 00:12:47,280 Speaker 1: it's a tough call. So why don't we do both? 244 00:12:47,840 --> 00:12:49,959 Speaker 1: All Right, We're gonna hand out two awards, right, We're 245 00:12:49,960 --> 00:12:52,160 Speaker 1: just gonna like dilute the value of our prizes by 246 00:12:52,200 --> 00:12:54,959 Speaker 1: giving out two of them. Make two categories, you know, 247 00:12:55,080 --> 00:12:59,439 Speaker 1: like the Peace Nobel Prize and the actual Nobel Prizes. 248 00:13:00,080 --> 00:13:03,679 Speaker 1: You mean the one in chemistry, right, That's exactly what 249 00:13:03,720 --> 00:13:06,160 Speaker 1: I was thinking. Yes, all right, so let's talk about 250 00:13:06,360 --> 00:13:10,040 Speaker 1: most massive star and also most I don't know, voluminous star, 251 00:13:11,800 --> 00:13:14,880 Speaker 1: biggest man, it is just biggest, most volume is just 252 00:13:14,920 --> 00:13:17,520 Speaker 1: the biggest. All right, so let's jump into it. I 253 00:13:17,559 --> 00:13:20,240 Speaker 1: guess what we talk about when we talk about mass. Yeah, well, 254 00:13:20,280 --> 00:13:22,400 Speaker 1: we had a fun podcast a week or so ago 255 00:13:22,520 --> 00:13:25,360 Speaker 1: about how massive stars can get, how big they can get, 256 00:13:25,480 --> 00:13:28,079 Speaker 1: how small they can get. And we also talked recently 257 00:13:28,080 --> 00:13:31,439 Speaker 1: about like where's the threshold between a planet and a star? 258 00:13:32,280 --> 00:13:35,720 Speaker 1: And really the definition of something that's a star is 259 00:13:35,760 --> 00:13:39,280 Speaker 1: something that confuse hydrogen, and in order for that to happen, 260 00:13:39,320 --> 00:13:41,360 Speaker 1: you just have to have enough mass, just like a 261 00:13:41,440 --> 00:13:44,640 Speaker 1: minimum mass threshold. You don't have enough stuff enough like 262 00:13:44,720 --> 00:13:48,679 Speaker 1: hydrogen gathered together and then compressed down, then you can't 263 00:13:48,679 --> 00:13:51,920 Speaker 1: get fusion going. And the minimum threshold there is something 264 00:13:52,080 --> 00:13:55,920 Speaker 1: like about a hundred times the mass of Jupiter. Doesn't 265 00:13:55,960 --> 00:13:59,719 Speaker 1: have to be hydrogen though, right, some stars confuse other elements. Yeah, 266 00:13:59,800 --> 00:14:03,280 Speaker 1: the heavier stuff like helium or carbon or neon or oxygen. 267 00:14:03,400 --> 00:14:06,000 Speaker 1: That takes even more mass in order to get that started. 268 00:14:06,080 --> 00:14:08,720 Speaker 1: But you're right, there is like a special category of 269 00:14:08,880 --> 00:14:13,240 Speaker 1: star called a brown dwarf that doesn't fuse hydrogen itself. 270 00:14:13,240 --> 00:14:17,360 Speaker 1: Iffuses an isotope of hydrogen called deuterium. So if you 271 00:14:17,400 --> 00:14:20,840 Speaker 1: have like fifty Jupiter masses or actually anything between about 272 00:14:20,880 --> 00:14:23,920 Speaker 1: like fifteen to eighty, you can get a form of 273 00:14:23,960 --> 00:14:27,320 Speaker 1: fusion going. It's called deuterium fusion. It's not like as 274 00:14:27,400 --> 00:14:30,760 Speaker 1: bright and as hot as normal hydrogen fusion. And so 275 00:14:30,760 --> 00:14:32,720 Speaker 1: this is I think a disagreement about whether or not 276 00:14:32,760 --> 00:14:36,080 Speaker 1: you would call this a star. Doesn't have regular hydrogen fusion, 277 00:14:36,280 --> 00:14:38,800 Speaker 1: so it's called a brown dwarf, also sometimes called a 278 00:14:38,920 --> 00:14:42,440 Speaker 1: failed star. And so the smallest thing you would really 279 00:14:42,480 --> 00:14:45,560 Speaker 1: call a star is about hundred times the mass of Jupiter, 280 00:14:45,840 --> 00:14:48,400 Speaker 1: and it can really fuse hydrogen, and you call these 281 00:14:48,480 --> 00:14:51,400 Speaker 1: red dwarfs. It's actually the most common kind of star 282 00:14:51,560 --> 00:14:54,640 Speaker 1: in the universe, these red dwarfs. They're everywhere, meaning like 283 00:14:54,680 --> 00:14:56,920 Speaker 1: if you take a hundred jupiters and you put them 284 00:14:56,920 --> 00:14:59,240 Speaker 1: on the same place, they will become a star. Yes, 285 00:14:59,280 --> 00:15:01,000 Speaker 1: if you took a to jupiters and put them all 286 00:15:01,000 --> 00:15:03,120 Speaker 1: in the same place, they would collapse and they would 287 00:15:03,120 --> 00:15:05,760 Speaker 1: start fusion. The interesting thing is that they actually wouldn't 288 00:15:05,800 --> 00:15:08,680 Speaker 1: be much bigger than Jupiter because there'd be so much 289 00:15:08,720 --> 00:15:11,640 Speaker 1: gravity would pull it together. So a red dwarf is 290 00:15:11,680 --> 00:15:14,400 Speaker 1: not actually bigger than Jupiter. It's just much more dense 291 00:15:14,440 --> 00:15:16,640 Speaker 1: that has a hundred times the mass, and that's enough 292 00:15:16,680 --> 00:15:19,720 Speaker 1: to get hydrogen fusion going. And what would they look 293 00:15:19,760 --> 00:15:21,920 Speaker 1: like if you saw them, Like, would they look as 294 00:15:21,920 --> 00:15:24,840 Speaker 1: bright as Arthen? No, they're not nearly as bright because 295 00:15:25,080 --> 00:15:27,600 Speaker 1: there's a very strong relationship between the mass of a 296 00:15:27,640 --> 00:15:30,040 Speaker 1: star and its brightness, and as the mass goes up, 297 00:15:30,160 --> 00:15:32,760 Speaker 1: the brightness increases by the power of four. So a 298 00:15:32,840 --> 00:15:35,280 Speaker 1: star that has like a tenth the mass of the 299 00:15:35,320 --> 00:15:38,400 Speaker 1: Sun has much much less brightness. It's like one ten 300 00:15:38,520 --> 00:15:41,000 Speaker 1: thousands of the brightness of the Sun. And in fact, 301 00:15:41,080 --> 00:15:44,200 Speaker 1: the closest red dwarf to Earth is called Bernard's Star, 302 00:15:44,600 --> 00:15:46,600 Speaker 1: is too dim to see by I even though it's 303 00:15:46,600 --> 00:15:50,000 Speaker 1: pretty close. Mmmmm, all right, So you take a hundred jupiters, 304 00:15:50,000 --> 00:15:51,920 Speaker 1: you put in together, you start fusing in the middle. 305 00:15:52,440 --> 00:15:55,360 Speaker 1: And is it basically like a more like a simmering 306 00:15:55,720 --> 00:15:57,840 Speaker 1: ball of fire, or is it only happening in the 307 00:15:57,880 --> 00:16:00,400 Speaker 1: core for example, it's definitely a ball of or like 308 00:16:00,440 --> 00:16:02,520 Speaker 1: if you were near you would get fried. It's still 309 00:16:02,640 --> 00:16:05,280 Speaker 1: very hot, it's just not nearly as bright as a 310 00:16:05,360 --> 00:16:09,200 Speaker 1: larger star, all right. So that's the minimum star. That's 311 00:16:09,240 --> 00:16:11,520 Speaker 1: the minimum star. And the amazing thing about the minimum 312 00:16:11,520 --> 00:16:14,880 Speaker 1: star is that remember that big stars burn hotter, and 313 00:16:14,880 --> 00:16:17,960 Speaker 1: so they burn faster. These small stars they're just sitting 314 00:16:17,960 --> 00:16:21,160 Speaker 1: there like glowing embers, and they're gonna last a long 315 00:16:21,320 --> 00:16:24,160 Speaker 1: long time. Like these red dwarves, they could last for 316 00:16:24,280 --> 00:16:28,280 Speaker 1: ten trillion years, ten trillion years and would never run 317 00:16:28,320 --> 00:16:31,000 Speaker 1: out of fuel or anything. Yeah, because they're just very 318 00:16:31,080 --> 00:16:33,800 Speaker 1: slowly burning their fuel. They're much cooler than our sun, 319 00:16:34,000 --> 00:16:36,200 Speaker 1: which is why they're much less bright, and so they're 320 00:16:36,200 --> 00:16:39,320 Speaker 1: sort of like conserving our fuel. The biggest, brightest stars 321 00:16:39,320 --> 00:16:42,160 Speaker 1: will only last like a few million years. The smaller 322 00:16:42,240 --> 00:16:44,400 Speaker 1: stars that are not as big and not as hot, 323 00:16:44,640 --> 00:16:46,880 Speaker 1: they can go on for trillions of years, much much 324 00:16:46,920 --> 00:16:50,880 Speaker 1: longer than the age of our universe so far. They're 325 00:16:50,920 --> 00:16:53,200 Speaker 1: like those TV actors that get work forever on TV, 326 00:16:53,280 --> 00:16:55,360 Speaker 1: but they're they're not as they don't shine as brightly 327 00:16:55,400 --> 00:16:59,760 Speaker 1: on the big screen. That's right, Christopher Walking, for example, No, 328 00:16:59,880 --> 00:17:02,720 Speaker 1: my Colcaine, that guy is still working, all right. Well, 329 00:17:02,880 --> 00:17:05,360 Speaker 1: so that's the minimum star, and so let's crank up 330 00:17:05,400 --> 00:17:08,800 Speaker 1: the mass style and get into more massive stars and 331 00:17:08,800 --> 00:17:12,280 Speaker 1: then we'll get to the actual biggest stars. But first 332 00:17:13,240 --> 00:17:27,960 Speaker 1: let's take a quick break, all right, Daniel, we're on 333 00:17:28,040 --> 00:17:31,280 Speaker 1: the hunt for the most massive stars in the universe, 334 00:17:31,720 --> 00:17:35,840 Speaker 1: and also the biggest stars in the universe, physical stars, 335 00:17:35,880 --> 00:17:38,640 Speaker 1: like the shiny kind that's out in space as through 336 00:17:38,720 --> 00:17:42,840 Speaker 1: physical stars, unless you're suggesting that Hollywood celebrities are non physical, 337 00:17:42,960 --> 00:17:49,000 Speaker 1: that they're like supernatural. They're very ithereal they transcend physcality, 338 00:17:49,760 --> 00:17:52,440 Speaker 1: that's right. So the next thing up after red dwarfs 339 00:17:52,440 --> 00:17:55,200 Speaker 1: are stars like our Sun, would you call a yellow dwarf? 340 00:17:55,960 --> 00:17:58,960 Speaker 1: And our son Like it's not nearly the biggest or 341 00:17:59,040 --> 00:18:02,080 Speaker 1: most massive star in the universe, but it's huge, you know, 342 00:18:02,119 --> 00:18:04,679 Speaker 1: compared to the size of the Earth, which already is 343 00:18:04,720 --> 00:18:08,960 Speaker 1: like staggeringly large, the Sun is enormous. It's like three 344 00:18:09,080 --> 00:18:11,880 Speaker 1: hundred thousand times the massive the Earth, and you could 345 00:18:11,880 --> 00:18:15,479 Speaker 1: fit more than a million earths inside of it. Mm hmmmm. 346 00:18:15,720 --> 00:18:18,679 Speaker 1: And that one is also fusion, right, definitely, this fusion 347 00:18:18,720 --> 00:18:21,359 Speaker 1: happening at the core of the Sun. Mm hmmm. Yeah, 348 00:18:21,560 --> 00:18:23,679 Speaker 1: and it's sort of just right for us though, right, Like, 349 00:18:23,720 --> 00:18:26,040 Speaker 1: if it was brighter, maybe we wouldn't be a lot 350 00:18:26,200 --> 00:18:29,120 Speaker 1: were dimmer. Yeah, exactly. If it was a lot brighter 351 00:18:29,119 --> 00:18:31,760 Speaker 1: than the surface of the Earth would be a lot toastier, 352 00:18:31,880 --> 00:18:34,000 Speaker 1: and maybe Mars would be a better neighborhood to live in. 353 00:18:34,280 --> 00:18:38,120 Speaker 1: So it's like three hundred times brighter than those red 354 00:18:38,200 --> 00:18:41,200 Speaker 1: dwarfs that are nearby, but it's only gonna last about 355 00:18:41,240 --> 00:18:43,879 Speaker 1: ten billion years. So we're halfway through the life of 356 00:18:43,880 --> 00:18:47,080 Speaker 1: the Sun. Oh wow, So it's about three hundred times 357 00:18:47,119 --> 00:18:51,280 Speaker 1: bigger than the red dwarf but will last much much less. Yeah, 358 00:18:51,280 --> 00:18:53,680 Speaker 1: so it's only about ten times the mass, but it's 359 00:18:53,680 --> 00:18:56,320 Speaker 1: gonna last a lot less time because if you crank 360 00:18:56,359 --> 00:18:58,920 Speaker 1: up the temperature, fusion really takes off and starts burning 361 00:18:58,960 --> 00:19:02,320 Speaker 1: a lot faster. It's very nonlinear. You double the mass, 362 00:19:02,440 --> 00:19:04,720 Speaker 1: you get much hotter temperatures, and you burn through that 363 00:19:04,760 --> 00:19:08,080 Speaker 1: mass much faster. So here in our solar system, that 364 00:19:08,119 --> 00:19:10,679 Speaker 1: means we're sort of on the low end of the 365 00:19:10,840 --> 00:19:14,159 Speaker 1: massive sun scale, right, our sun is relatively small compared 366 00:19:14,200 --> 00:19:16,959 Speaker 1: to what's out there. Yes, absolutely, our sun is not 367 00:19:17,080 --> 00:19:19,920 Speaker 1: impressive compared to the most massive stars that are out there. 368 00:19:20,160 --> 00:19:22,399 Speaker 1: It's not in the population of the smallest stars, the 369 00:19:22,440 --> 00:19:24,679 Speaker 1: red dwarfs that are very, very common. But it's not 370 00:19:24,760 --> 00:19:27,920 Speaker 1: an impressive star at all. We still like it though. 371 00:19:28,160 --> 00:19:31,000 Speaker 1: It's still our favorite star. It's perfect for us, all right. 372 00:19:31,040 --> 00:19:33,280 Speaker 1: So let's crack up the mass even more. What happens 373 00:19:33,400 --> 00:19:35,879 Speaker 1: if you get into thousands of times the mass of 374 00:19:35,880 --> 00:19:38,679 Speaker 1: our Sun? Well you can't. Actually, it turns out that 375 00:19:38,760 --> 00:19:41,600 Speaker 1: the biggest stars that are out there are only like 376 00:19:41,760 --> 00:19:45,360 Speaker 1: a hundred hundred fifty up to maybe about two hundred 377 00:19:45,400 --> 00:19:49,600 Speaker 1: times the mass of the Sun. I see, because what 378 00:19:49,640 --> 00:19:52,119 Speaker 1: happens after that. What happens after that is that the 379 00:19:52,160 --> 00:19:55,720 Speaker 1: Sun gets really big and really hot, and it starts 380 00:19:55,760 --> 00:19:59,200 Speaker 1: to burn really strongly is core, and that fusion generates 381 00:19:59,240 --> 00:20:01,399 Speaker 1: a lot of radiation, and so it blows out the 382 00:20:01,440 --> 00:20:03,479 Speaker 1: outer layers of the star. So there's sort of an 383 00:20:03,560 --> 00:20:06,240 Speaker 1: upper limit to how much mass you can cram into 384 00:20:06,280 --> 00:20:08,520 Speaker 1: a star and how it still be stable. Remember, a 385 00:20:08,560 --> 00:20:11,320 Speaker 1: star is sort of a balance between gravity that's trying 386 00:20:11,359 --> 00:20:14,760 Speaker 1: to compact it and fusion that's pushing out the glowing 387 00:20:14,800 --> 00:20:18,080 Speaker 1: the hot energy that's keeping it from compacting. I see. 388 00:20:18,119 --> 00:20:20,879 Speaker 1: So if you gather more than two hundred times the 389 00:20:20,920 --> 00:20:23,919 Speaker 1: mass of our Sun together in like a giant hydrogen cloud, 390 00:20:24,560 --> 00:20:27,080 Speaker 1: it wouldn't all crunch together in the middle because by 391 00:20:27,080 --> 00:20:30,200 Speaker 1: the time it starts to crunch, the middle starts exploding, 392 00:20:30,240 --> 00:20:32,320 Speaker 1: and then that blows everything away. Yeah, and first of all, 393 00:20:32,320 --> 00:20:34,760 Speaker 1: if you have such a huge cloud, it probably wouldn't 394 00:20:34,760 --> 00:20:37,640 Speaker 1: collapse into just one star. It's more likely to collapse 395 00:20:37,640 --> 00:20:40,919 Speaker 1: into several smaller stars. But if you somehow arranged like 396 00:20:41,160 --> 00:20:44,240 Speaker 1: a bunch of really big stars to combine themselves together 397 00:20:44,280 --> 00:20:46,679 Speaker 1: into something which was two or three hundred times the 398 00:20:46,680 --> 00:20:49,000 Speaker 1: mass of the Sun, it would blow itself apart because 399 00:20:49,000 --> 00:20:52,160 Speaker 1: the fusion at its core would be so powerful. All right, well, 400 00:20:52,240 --> 00:20:54,760 Speaker 1: let's take the next step. Then, what's next step? After 401 00:20:54,840 --> 00:20:58,399 Speaker 1: our star? After our star? This serious which is actually 402 00:20:58,440 --> 00:21:01,840 Speaker 1: the brightest star in night sky, and it has two 403 00:21:01,960 --> 00:21:04,560 Speaker 1: times the mass of our Sun, so it's like two 404 00:21:04,600 --> 00:21:08,320 Speaker 1: scoops of suns, and it's much bigger actually than our son. 405 00:21:08,359 --> 00:21:10,920 Speaker 1: It's like eight times the volume. And even though it's 406 00:21:10,920 --> 00:21:14,640 Speaker 1: only twice the mass, it's like twenty five times brighter 407 00:21:14,880 --> 00:21:18,240 Speaker 1: than our sun. That's a general thing, or is it 408 00:21:18,320 --> 00:21:21,040 Speaker 1: just this one star? Now? In general? As you crank 409 00:21:21,119 --> 00:21:23,840 Speaker 1: up the mass, the brightness goes up much much faster. 410 00:21:24,119 --> 00:21:26,680 Speaker 1: This is the mass luminosity relationship we talked about in 411 00:21:26,680 --> 00:21:29,560 Speaker 1: another podcast episode. That's what we use actually to measure 412 00:21:29,560 --> 00:21:31,920 Speaker 1: the massive stars. We look at their brightness because, as 413 00:21:31,920 --> 00:21:34,600 Speaker 1: we said before, as you add mass, the temperature increases, 414 00:21:34,760 --> 00:21:37,800 Speaker 1: and it increases really dramatically, which tips off nuclear fusion, 415 00:21:37,920 --> 00:21:41,240 Speaker 1: which makes things even brighter. M Yeah. In fact, the 416 00:21:41,240 --> 00:21:43,440 Speaker 1: brightest star in our night sky is one of these 417 00:21:43,480 --> 00:21:47,760 Speaker 1: two suns. Starts. Yeah, exactly, that's serious. Are you serious? 418 00:21:49,680 --> 00:21:53,719 Speaker 1: Surely you're joking and stop calling me Shirlett. Alright, So 419 00:21:53,840 --> 00:21:55,960 Speaker 1: a star that's two times the massive our sun would 420 00:21:56,000 --> 00:21:58,719 Speaker 1: only live two and a half billion years. Yeah, wow, 421 00:21:58,880 --> 00:22:01,840 Speaker 1: it's burned through his fuel, all right, what's the next step? 422 00:22:01,960 --> 00:22:05,680 Speaker 1: Next step up is Beta Centauri. This thing is twelve 423 00:22:05,840 --> 00:22:08,159 Speaker 1: times the mass of the Sun and it's about a 424 00:22:08,320 --> 00:22:11,040 Speaker 1: thousand times as big. So you could take our son 425 00:22:11,119 --> 00:22:14,160 Speaker 1: and fitted into this star a thousand times. It's hard 426 00:22:14,200 --> 00:22:17,400 Speaker 1: to hold that idea in your mind. Wow, it's only 427 00:22:17,440 --> 00:22:20,639 Speaker 1: like ten times more massive, but it creates such a 428 00:22:20,680 --> 00:22:24,440 Speaker 1: crazy condition of explosions that that sun basically flows up right, 429 00:22:24,800 --> 00:22:27,320 Speaker 1: It's like a big fire exactly. It's a huge fire, 430 00:22:27,359 --> 00:22:31,120 Speaker 1: and that's why it's twenty thousand times brighter than our sun. 431 00:22:31,480 --> 00:22:36,040 Speaker 1: Twenty thousand times. Wow, that's like taking twenty sons and 432 00:22:36,080 --> 00:22:39,359 Speaker 1: shining it on us. Imagine having twenty thousand sons in 433 00:22:39,400 --> 00:22:42,280 Speaker 1: the sky like that's a hot day. Yeah, we need 434 00:22:42,280 --> 00:22:46,480 Speaker 1: twenty thousand SPF at least. And this is a super 435 00:22:46,520 --> 00:22:49,520 Speaker 1: awesome star because it's only going to live for twenty 436 00:22:49,640 --> 00:22:53,560 Speaker 1: million years. These things, they are fiery, they're impressive, but 437 00:22:53,680 --> 00:22:57,199 Speaker 1: they do not stick around. What happens after twenty million years. 438 00:22:57,240 --> 00:23:00,119 Speaker 1: After twenty million years, it goes into its super giant is. 439 00:23:00,119 --> 00:23:03,000 Speaker 1: It actually gets much much bigger and then eventually collapses 440 00:23:03,040 --> 00:23:05,359 Speaker 1: and it's going to form either a neutron star or 441 00:23:05,400 --> 00:23:08,640 Speaker 1: a black hole, depending exactly on how much mass it has. Wow, 442 00:23:08,840 --> 00:23:10,919 Speaker 1: don't you mean in years is not a lot of 443 00:23:10,960 --> 00:23:14,119 Speaker 1: time astronomically speaking, right, you wouldn't have enough time to 444 00:23:14,880 --> 00:23:18,040 Speaker 1: develop life for really, you know, get all your grocery 445 00:23:18,040 --> 00:23:20,520 Speaker 1: shopping done. No, you wouldn't. And the other interesting thing 446 00:23:20,600 --> 00:23:22,480 Speaker 1: is that this is part of a star system that 447 00:23:22,520 --> 00:23:25,639 Speaker 1: has three stars. You've heard of a binary star system. 448 00:23:25,680 --> 00:23:27,920 Speaker 1: We have two stars orbiting each other. This one's part 449 00:23:27,960 --> 00:23:30,800 Speaker 1: of a triple system. So there are two other stars 450 00:23:30,800 --> 00:23:33,320 Speaker 1: there that are much smaller that will last longer, and 451 00:23:33,359 --> 00:23:35,640 Speaker 1: you might develop life around one of those, but only 452 00:23:35,720 --> 00:23:39,199 Speaker 1: if it can survive the cataclysmic end of Bitta Centaur. 453 00:23:40,760 --> 00:23:42,840 Speaker 1: How common are these types of stars? Are we getting 454 00:23:42,920 --> 00:23:46,000 Speaker 1: too more rare kinds of stars? These are definitely much 455 00:23:46,000 --> 00:23:48,480 Speaker 1: more rare. As the mass goes up, the frequency that 456 00:23:48,480 --> 00:23:51,639 Speaker 1: you'll find these stars drops, not just because it's harder 457 00:23:51,680 --> 00:23:54,360 Speaker 1: to get a large blob of mass, it's just less 458 00:23:54,400 --> 00:23:56,520 Speaker 1: likely for it to happen, but also because they don't 459 00:23:56,560 --> 00:23:59,080 Speaker 1: last very long. Like these red dwarfs, they're gonna be 460 00:23:59,119 --> 00:24:02,520 Speaker 1: around basically for ever, right, trillions of years. The yellow 461 00:24:02,560 --> 00:24:04,920 Speaker 1: doors we're talking about billions of years about the lifetime 462 00:24:04,960 --> 00:24:07,880 Speaker 1: of the universe. Here, we're just talking about millions of years, 463 00:24:07,880 --> 00:24:10,600 Speaker 1: which astronomically speaking, is like a blink. So these things, 464 00:24:10,600 --> 00:24:12,680 Speaker 1: when they do happen, they don't stick around very long, 465 00:24:12,680 --> 00:24:16,399 Speaker 1: and that of course contributes to their rareness. M All right, 466 00:24:16,480 --> 00:24:19,280 Speaker 1: let's get into the King of all or queen of 467 00:24:19,320 --> 00:24:22,119 Speaker 1: all massive stars. There is one that you can crown 468 00:24:22,160 --> 00:24:24,560 Speaker 1: as the most massive star there is, though there is 469 00:24:24,600 --> 00:24:27,120 Speaker 1: some disagreement. You know, it's hard to measure these things, 470 00:24:27,160 --> 00:24:29,800 Speaker 1: as we talked about, especially on the very upper edge, 471 00:24:29,840 --> 00:24:32,560 Speaker 1: and so different astronomers might say that different stars are 472 00:24:32,680 --> 00:24:35,280 Speaker 1: the most massive. But there's a couple that are like 473 00:24:35,440 --> 00:24:37,480 Speaker 1: right at the edge. And the one I think that's 474 00:24:37,480 --> 00:24:40,760 Speaker 1: super cool is this one called are one three six 475 00:24:40,960 --> 00:24:44,639 Speaker 1: A one. This one's two hundred and fifteen times the 476 00:24:44,680 --> 00:24:48,000 Speaker 1: mass of the Sun, two hundred and fifteen serving scoops 477 00:24:48,040 --> 00:24:51,720 Speaker 1: all put together into one star. Wow, And I imagine 478 00:24:51,760 --> 00:24:54,760 Speaker 1: that's really bright. Yeah, this thing is as bright as 479 00:24:54,880 --> 00:25:02,960 Speaker 1: nine million sons nine millions Sun's shining all at once. Yeah. 480 00:25:03,240 --> 00:25:05,680 Speaker 1: And it's so close to this limit at how big 481 00:25:05,720 --> 00:25:07,440 Speaker 1: a star can be that it's just not going to 482 00:25:07,600 --> 00:25:10,800 Speaker 1: last very long. It's radiating out so much energy that 483 00:25:10,880 --> 00:25:13,480 Speaker 1: the fusion happening at its core is pushing out the 484 00:25:13,600 --> 00:25:17,080 Speaker 1: edges of the star. It's losing mass constantly. It's an explosion. 485 00:25:17,119 --> 00:25:20,480 Speaker 1: It's falling apart mm because at some point it like 486 00:25:20,560 --> 00:25:24,360 Speaker 1: pushes things out so far that they just escaped the gravity. Yeah, exactly. 487 00:25:24,359 --> 00:25:27,359 Speaker 1: The fusion pressure at the surface is greater than the 488 00:25:27,400 --> 00:25:30,560 Speaker 1: gravitational hold though. Things are getting pushed away from the 489 00:25:30,600 --> 00:25:33,480 Speaker 1: star like you imagine these really really massive objects in 490 00:25:33,520 --> 00:25:35,760 Speaker 1: space are going to suck you in. Right, this is 491 00:25:35,760 --> 00:25:38,840 Speaker 1: the star that pushes you away. The solar wind from 492 00:25:38,840 --> 00:25:41,320 Speaker 1: this star is so strong that it's actually pushing its 493 00:25:41,359 --> 00:25:46,280 Speaker 1: own skin off. Wow. That's disgusting but also pretty impressive. 494 00:25:46,520 --> 00:25:49,240 Speaker 1: Don't be judgmental, man, That's just the way the stars are. 495 00:25:49,359 --> 00:25:51,280 Speaker 1: And when you say pushing you, you really mean more 496 00:25:51,320 --> 00:25:53,920 Speaker 1: like frying you, right, Like, if you're there being pushed 497 00:25:53,920 --> 00:25:55,920 Speaker 1: by the star, it's not like it's pushing you, it's 498 00:25:55,920 --> 00:25:58,520 Speaker 1: like it's throwing fire at you. Well, both, Like, it's 499 00:25:58,560 --> 00:26:01,200 Speaker 1: a lot of energy for you to remember, the solar 500 00:26:01,240 --> 00:26:04,600 Speaker 1: wind has momentum. That's how we talk about like solar sails, right. 501 00:26:04,640 --> 00:26:07,600 Speaker 1: They can really capture the momentum of the solar wind, 502 00:26:07,760 --> 00:26:10,000 Speaker 1: and that's why these things are expanding. That's why they're 503 00:26:10,080 --> 00:26:13,000 Speaker 1: literally blowing up because the solar wind is literally pushing, 504 00:26:13,240 --> 00:26:15,920 Speaker 1: not just frying and cooking. There's a lot of momentum 505 00:26:15,920 --> 00:26:18,480 Speaker 1: that's being imparted anything that comes close to this thing, 506 00:26:18,640 --> 00:26:22,200 Speaker 1: and actually the outer layers, so it's tearing itself apart. Right. 507 00:26:22,280 --> 00:26:23,960 Speaker 1: I guess what I mean is it wouldn't feel good 508 00:26:23,960 --> 00:26:26,880 Speaker 1: to be pushed by that much radiation. No, it would 509 00:26:26,880 --> 00:26:29,399 Speaker 1: not feel good. I don't recommend going like solar surfing 510 00:26:29,480 --> 00:26:35,280 Speaker 1: or anything sailing. The incredible thing is that this is 511 00:26:35,359 --> 00:26:38,800 Speaker 1: just one part of an enormous cluster. Like this is 512 00:26:39,040 --> 00:26:42,160 Speaker 1: maybe the most massive star in the universe, nine million 513 00:26:42,200 --> 00:26:45,399 Speaker 1: times brighter than the Sun. But actually only recently we 514 00:26:45,440 --> 00:26:48,159 Speaker 1: figured out that it's one star because it's part of 515 00:26:48,200 --> 00:26:52,520 Speaker 1: this big blob of stars that together, this huge cluster 516 00:26:52,600 --> 00:26:55,800 Speaker 1: is called R one three six, is ten thousand times 517 00:26:55,840 --> 00:26:59,760 Speaker 1: brighter than just this star. Oh wow, this most massive 518 00:26:59,760 --> 00:27:02,800 Speaker 1: star is really like the minor player in an orchestra 519 00:27:02,960 --> 00:27:05,600 Speaker 1: of stars. Yeah, it's the biggest one. It's just a 520 00:27:05,720 --> 00:27:08,680 Speaker 1: huge collection of stars, and this is like the big 521 00:27:08,720 --> 00:27:12,120 Speaker 1: grand Pappy. But together all those stars outshine this one 522 00:27:12,200 --> 00:27:16,840 Speaker 1: by ten. So it's a crazy object out there. Is 523 00:27:16,840 --> 00:27:19,399 Speaker 1: that about as massive as stars can get. What if 524 00:27:19,440 --> 00:27:21,920 Speaker 1: I have a star that massive and I pumped more 525 00:27:22,200 --> 00:27:25,880 Speaker 1: hydrogen into it, what would happen? It would blow itself up. 526 00:27:26,040 --> 00:27:28,080 Speaker 1: As you get it more massive, it's going to increase 527 00:27:28,160 --> 00:27:30,639 Speaker 1: the temperature and that's going to increase the rate of fusion, 528 00:27:30,680 --> 00:27:33,119 Speaker 1: which is an increase the radiation and pressure, and so 529 00:27:33,160 --> 00:27:36,239 Speaker 1: it's going to tear itself apart. It's gonna blow up, 530 00:27:36,480 --> 00:27:38,879 Speaker 1: It's gonna blow up. Yeah. Somebody actually wrote to me 531 00:27:38,920 --> 00:27:41,199 Speaker 1: and asked me, like, if you wanted to blow up 532 00:27:41,200 --> 00:27:45,639 Speaker 1: a star, what would be your go to strategy? And 533 00:27:45,760 --> 00:27:48,200 Speaker 1: you know, as usual, I thought, is this a supervillain 534 00:27:48,240 --> 00:27:51,720 Speaker 1: making a plan asking me for physics consulting? But the 535 00:27:51,760 --> 00:27:54,239 Speaker 1: answer I gave him I thought was pretty impractical, which was, like, 536 00:27:54,440 --> 00:27:56,280 Speaker 1: just add a lot of mass to the star. That 537 00:27:56,320 --> 00:27:58,480 Speaker 1: will blow it up. So if he's somehow capable of 538 00:27:58,480 --> 00:28:01,760 Speaker 1: injecting five times more mass into our sun, for example, 539 00:28:02,160 --> 00:28:05,000 Speaker 1: that would spell its doom. Right. Well, I mean, obviously 540 00:28:05,080 --> 00:28:06,560 Speaker 1: it's a lot, but it doesn't sound like a lot. 541 00:28:06,920 --> 00:28:09,040 Speaker 1: You don't need millions of suns to blow it up. 542 00:28:09,080 --> 00:28:11,320 Speaker 1: You can just gather a few hundred. Yeah, And it's fascinating. 543 00:28:11,359 --> 00:28:13,439 Speaker 1: That's why these extremes are really interesting. It tells you 544 00:28:13,520 --> 00:28:16,119 Speaker 1: that you can't have an arbitrarily sized star, right, You 545 00:28:16,119 --> 00:28:19,760 Speaker 1: can't just have an enormous galaxy size star. That's why 546 00:28:19,840 --> 00:28:22,840 Speaker 1: galaxies are filled with stars instead of us having galaxy 547 00:28:22,920 --> 00:28:25,880 Speaker 1: sized stars, because there's an upper limit. Because stars are 548 00:28:25,920 --> 00:28:28,840 Speaker 1: not just like blobs of gas floating out in space. 549 00:28:29,119 --> 00:28:32,760 Speaker 1: There's this push and pull. Gravity squeezing them down, fusion 550 00:28:32,800 --> 00:28:35,320 Speaker 1: is pushing them out, And there's only certain regimes in 551 00:28:35,320 --> 00:28:38,280 Speaker 1: which those two things are close enough to being balanced 552 00:28:38,280 --> 00:28:41,240 Speaker 1: that the thing can exist for very long at all. Right, 553 00:28:41,520 --> 00:28:44,680 Speaker 1: But I guess also that's only in the star category. 554 00:28:44,880 --> 00:28:47,520 Speaker 1: You can have objects that are more massive than two 555 00:28:47,640 --> 00:28:50,440 Speaker 1: or three hundred masses of the Sun, right, Yeah, for example, 556 00:28:50,440 --> 00:28:52,160 Speaker 1: a black hole. Right, you may have black holes that 557 00:28:52,200 --> 00:28:55,280 Speaker 1: are billion times the mass of the Sun. And we 558 00:28:55,360 --> 00:28:58,040 Speaker 1: talked about what's the biggest planet you can have to Yeah, 559 00:28:58,120 --> 00:29:00,960 Speaker 1: exactly though that's definitional, right, as far as we know, though, 560 00:29:00,960 --> 00:29:04,200 Speaker 1: there's no physical upper limit on the mass of a 561 00:29:04,240 --> 00:29:06,320 Speaker 1: black hole. The only limit there is how do you 562 00:29:06,440 --> 00:29:08,640 Speaker 1: get so much stuff near a black hole so that 563 00:29:08,680 --> 00:29:10,360 Speaker 1: he can eat it? And how does it actually fall 564 00:29:10,440 --> 00:29:12,520 Speaker 1: in within the lifetime of the universe, which is why 565 00:29:12,600 --> 00:29:15,560 Speaker 1: we think the biggest black holes out there are like five, ten, 566 00:29:16,080 --> 00:29:18,800 Speaker 1: maybe fifteen billion times in the mass of the Sun. 567 00:29:18,880 --> 00:29:20,320 Speaker 1: We don't see an the outh that there are a 568 00:29:20,400 --> 00:29:23,920 Speaker 1: trillion times the mass of the Sun, though theoretically there's 569 00:29:23,920 --> 00:29:27,120 Speaker 1: nothing preventing that from happening. But here, even theoretically, you 570 00:29:27,160 --> 00:29:30,080 Speaker 1: can't build a star that has five dred times the 571 00:29:30,120 --> 00:29:32,280 Speaker 1: mass of the Sun and expect it to last more 572 00:29:32,320 --> 00:29:35,360 Speaker 1: than a few hundred thousand years. Right, What if I 573 00:29:35,400 --> 00:29:38,320 Speaker 1: take like a harrier element? Can I take five hundred 574 00:29:38,360 --> 00:29:41,040 Speaker 1: times the mass of the Sun in helium and put 575 00:29:41,080 --> 00:29:43,800 Speaker 1: that together? Would that give me a star? No, because 576 00:29:43,800 --> 00:29:46,440 Speaker 1: that would also trigger fusion, and that fusion would be 577 00:29:46,440 --> 00:29:49,760 Speaker 1: even hotter and more energetic, and so you would also 578 00:29:50,080 --> 00:29:53,120 Speaker 1: just spell the death of the star. But the elements 579 00:29:53,120 --> 00:29:56,360 Speaker 1: would be heavier, wouldn't it, wouldn't there be more gravitational pressure. Yeah, 580 00:29:56,400 --> 00:29:59,840 Speaker 1: And more gravitational pressure is exactly what's driving the fusion. Right. 581 00:30:00,040 --> 00:30:03,959 Speaker 1: More gravitational pressure means higher temperatures, which means faster fusion, 582 00:30:04,160 --> 00:30:06,760 Speaker 1: which means more fusion radiation, which means the death of 583 00:30:06,760 --> 00:30:10,880 Speaker 1: your star. All right, so there's a limit to start them. 584 00:30:11,040 --> 00:30:14,120 Speaker 1: There is a limit to start them. Exactly about Tom Cruise. 585 00:30:14,160 --> 00:30:17,440 Speaker 1: You can't get any bigger than that, Tom Hanks, Tom Cruise, 586 00:30:17,520 --> 00:30:20,520 Speaker 1: Nicole Kidman, that's it. You collapse into an egotistical black 587 00:30:20,560 --> 00:30:25,360 Speaker 1: hole after that black hole of paparazzis and and tabloids. Exactly. 588 00:30:25,640 --> 00:30:28,040 Speaker 1: All right, Well that's the most massive stars. Now let's 589 00:30:28,080 --> 00:30:30,560 Speaker 1: get to the question of what's the biggest star, Like, 590 00:30:30,600 --> 00:30:33,000 Speaker 1: if you're standing in front of it, what would be 591 00:30:33,040 --> 00:30:35,120 Speaker 1: the biggest star that you can see or be in 592 00:30:35,120 --> 00:30:37,360 Speaker 1: the presence of. So let's get into that, but first 593 00:30:37,400 --> 00:30:51,840 Speaker 1: let's take a quick break. All right, we're talking about 594 00:30:51,880 --> 00:30:56,520 Speaker 1: the biggest star in the universe, not just here on 595 00:30:56,560 --> 00:30:59,960 Speaker 1: Earth as a movie star, but in the astronomical sense. 596 00:31:00,240 --> 00:31:03,040 Speaker 1: What's the largest right, that's what we're talking about now, 597 00:31:03,240 --> 00:31:05,800 Speaker 1: largest star that you can have, Like, if you're standing 598 00:31:05,840 --> 00:31:07,600 Speaker 1: in front of it, what's the biggest thing that you 599 00:31:07,640 --> 00:31:10,560 Speaker 1: could be looking at? What takes up the most space 600 00:31:10,640 --> 00:31:13,080 Speaker 1: in our universe? I like to imagine, you know, taking 601 00:31:13,080 --> 00:31:15,480 Speaker 1: a spaceship and going up to the surface of the Sun. 602 00:31:15,760 --> 00:31:18,440 Speaker 1: It would seem like it filled up your whole horizon, right, 603 00:31:18,440 --> 00:31:21,400 Speaker 1: It would be so vast, like an ocean of burning plasma. 604 00:31:22,360 --> 00:31:24,560 Speaker 1: And then it's awesome to think about like that being 605 00:31:24,640 --> 00:31:28,360 Speaker 1: dwarfed by something even larger, right right, all right, So 606 00:31:28,400 --> 00:31:31,400 Speaker 1: then let's talk about volume, like what determines the volume 607 00:31:31,440 --> 00:31:34,080 Speaker 1: of a star. This is a little bit tricky, right, 608 00:31:34,120 --> 00:31:36,360 Speaker 1: Like how you measure the volume of the star and 609 00:31:36,400 --> 00:31:38,800 Speaker 1: how you even define it is a little bit tricky. 610 00:31:39,080 --> 00:31:41,600 Speaker 1: Don't suns have a surface that you can measure off of, 611 00:31:41,760 --> 00:31:43,880 Speaker 1: like our sons has a surface, right, pictures of it 612 00:31:43,920 --> 00:31:46,200 Speaker 1: looked like it has an edge. Yeah, but it's sort 613 00:31:46,240 --> 00:31:49,040 Speaker 1: of like the Earth, like where it is the atmosphere end. 614 00:31:49,320 --> 00:31:51,160 Speaker 1: It's not a hard cut off. It's sort of like 615 00:31:51,480 --> 00:31:54,080 Speaker 1: drifts off gradually. So you can say, obviously we have 616 00:31:54,120 --> 00:31:56,120 Speaker 1: a surface on the Earth, but the Sun doesn't have 617 00:31:56,160 --> 00:31:58,360 Speaker 1: a rigid surface the same way the Earth does. It 618 00:31:58,440 --> 00:32:01,480 Speaker 1: sort of has a gradual draw off in density. Then 619 00:32:01,480 --> 00:32:03,280 Speaker 1: you get to the outer layers, and so it's hard 620 00:32:03,320 --> 00:32:07,120 Speaker 1: to know exactly where to define the size of the star. Right, 621 00:32:07,120 --> 00:32:09,120 Speaker 1: It's a little fuzzy, but still I feel like, you know, 622 00:32:09,200 --> 00:32:10,680 Speaker 1: if you look at a picture of the Sun that 623 00:32:10,760 --> 00:32:13,400 Speaker 1: they've taken, it does seem to have like a surface 624 00:32:13,440 --> 00:32:17,520 Speaker 1: of molten something or the surface of fire, after which 625 00:32:17,600 --> 00:32:20,160 Speaker 1: it's not as defined, or you see the blackness of 626 00:32:20,160 --> 00:32:22,080 Speaker 1: space behind it. And you can also think about, like 627 00:32:22,160 --> 00:32:24,840 Speaker 1: what is the part of the star that's actually glowing, 628 00:32:24,920 --> 00:32:27,480 Speaker 1: that's giving off light. Maybe you could define the edge 629 00:32:27,480 --> 00:32:30,120 Speaker 1: of it that way, And that's actually useful because that's 630 00:32:30,160 --> 00:32:33,280 Speaker 1: connected to how we know the size of these stars. 631 00:32:33,520 --> 00:32:35,400 Speaker 1: Like we're gonna talk about some really big stars that 632 00:32:35,440 --> 00:32:37,880 Speaker 1: are super far away, and you might wonder, like, well, 633 00:32:37,920 --> 00:32:40,440 Speaker 1: how do we know this thing is so big and 634 00:32:40,480 --> 00:32:43,480 Speaker 1: we can't measure it exactly? Only for like really close 635 00:32:43,560 --> 00:32:46,560 Speaker 1: up stars, can we actually resolve the left side of 636 00:32:46,560 --> 00:32:48,520 Speaker 1: it and the right side of it make a measurement 637 00:32:48,800 --> 00:32:50,840 Speaker 1: directly of how big it is. It only works for 638 00:32:50,880 --> 00:32:53,120 Speaker 1: stars that are very very close to us, where we 639 00:32:53,120 --> 00:32:55,600 Speaker 1: can use like parallax. Beyond that, we have to have 640 00:32:55,720 --> 00:32:58,720 Speaker 1: models that say, if the star is this temperature and 641 00:32:58,800 --> 00:33:01,400 Speaker 1: has this brightness, and that tells us it must have 642 00:33:01,440 --> 00:33:04,360 Speaker 1: a certain surface area in order to emit that much light, 643 00:33:04,640 --> 00:33:07,120 Speaker 1: and from that we can deduce the volume of the star. 644 00:33:08,480 --> 00:33:10,840 Speaker 1: You have to basically sort of guests based on your 645 00:33:10,880 --> 00:33:13,600 Speaker 1: knowledge of how sounds work. Yeah, we have a model 646 00:33:13,720 --> 00:33:16,080 Speaker 1: who is not exactly a guess. It's called nuclear physics. 647 00:33:16,240 --> 00:33:18,160 Speaker 1: But we have a model for what's going on inside 648 00:33:18,160 --> 00:33:20,640 Speaker 1: the star that connects the brightness of the star with 649 00:33:20,720 --> 00:33:22,560 Speaker 1: the mass of the star and the temperature of the star, 650 00:33:22,680 --> 00:33:25,280 Speaker 1: and from all that we can estimate what the radius 651 00:33:25,280 --> 00:33:27,160 Speaker 1: of the star must be. I feel like I just 652 00:33:27,200 --> 00:33:30,560 Speaker 1: insulted you. Then you not just me It's okay, It's 653 00:33:30,560 --> 00:33:33,000 Speaker 1: just a whole field of physics. You mean, a hypothesis 654 00:33:33,000 --> 00:33:36,080 Speaker 1: without proof is not a guess. It's not without proof. 655 00:33:36,360 --> 00:33:38,239 Speaker 1: We develop these models and we test them. We look 656 00:33:38,280 --> 00:33:40,200 Speaker 1: at in the universe and we see do the stars 657 00:33:40,240 --> 00:33:42,600 Speaker 1: behave the way we expect? And we can only test 658 00:33:42,600 --> 00:33:44,800 Speaker 1: them in some cases for closer up stars, And the 659 00:33:44,880 --> 00:33:47,320 Speaker 1: rest of it is extrapolation. But it's not just like, 660 00:33:47,800 --> 00:33:49,960 Speaker 1: I don't know, let's pick a number. So there are 661 00:33:49,960 --> 00:33:53,120 Speaker 1: stars that we can measure the size of from here. Yeah, 662 00:33:53,160 --> 00:33:55,000 Speaker 1: there's stars that are close enough that we can use 663 00:33:55,040 --> 00:33:58,360 Speaker 1: parallax to directly measure their size, but not very many. 664 00:34:00,560 --> 00:34:03,239 Speaker 1: Al right. Well, the other tricky thing is that the 665 00:34:03,320 --> 00:34:05,800 Speaker 1: size of a star changes over its life. You know, 666 00:34:05,800 --> 00:34:09,080 Speaker 1: it grows and then it shrinks. Yeah, exactly. The star 667 00:34:09,440 --> 00:34:11,800 Speaker 1: for most of its life is about the same size. 668 00:34:11,840 --> 00:34:15,080 Speaker 1: It burns happily, it's in that's happy place where fusion 669 00:34:15,520 --> 00:34:18,360 Speaker 1: and gravity are like in balance with each other. But 670 00:34:18,400 --> 00:34:21,919 Speaker 1: eventually fusion makes really heavy metals which collected the core 671 00:34:21,960 --> 00:34:25,200 Speaker 1: of the star and increase the gravity, and then eventually 672 00:34:25,200 --> 00:34:27,680 Speaker 1: the fusion starts happening sort of more on the outer 673 00:34:27,880 --> 00:34:30,400 Speaker 1: edges of the star. You only have hydrogen near the 674 00:34:30,440 --> 00:34:32,399 Speaker 1: outer edges of the star now, and so that's where 675 00:34:32,520 --> 00:34:35,720 Speaker 1: most of the hydrogen fusion is happening, and that creates 676 00:34:35,760 --> 00:34:38,279 Speaker 1: more pressure to blow out the star, makes it get 677 00:34:38,440 --> 00:34:40,960 Speaker 1: much much bigger. Our Sun, for example, is going to 678 00:34:41,040 --> 00:34:44,440 Speaker 1: get to two hundred times its current volume when it 679 00:34:44,480 --> 00:34:49,040 Speaker 1: goes into its red super giant phase. Mmm. Right. It 680 00:34:49,120 --> 00:34:52,520 Speaker 1: gets so hot that it burns brighter and bigger. Basically 681 00:34:52,520 --> 00:34:55,280 Speaker 1: the flame gets bigger, yeah, exactly, and so it gets 682 00:34:55,320 --> 00:34:58,480 Speaker 1: really big and fluffy. And like where the Earth is 683 00:34:58,600 --> 00:35:01,640 Speaker 1: right now is probably gonna be pretty close to the 684 00:35:01,760 --> 00:35:04,200 Speaker 1: radius of the Sun when it gets near the end 685 00:35:04,239 --> 00:35:06,640 Speaker 1: of its life cycle. That's in about five billion years, 686 00:35:06,640 --> 00:35:08,720 Speaker 1: so you still got time to do a lot of stuff. 687 00:35:09,120 --> 00:35:11,200 Speaker 1: But that's going to happen to our star and to 688 00:35:11,280 --> 00:35:14,560 Speaker 1: almost every star out there, all right, So I guess 689 00:35:14,560 --> 00:35:17,680 Speaker 1: maybe we're really talking about what's the peak volume of 690 00:35:17,800 --> 00:35:20,279 Speaker 1: stars right like at their biggest what's the biggest they 691 00:35:20,280 --> 00:35:22,919 Speaker 1: can get exactly? Or like when we look out there 692 00:35:23,000 --> 00:35:25,719 Speaker 1: currently in the universe, what are the biggest stars that 693 00:35:25,760 --> 00:35:27,920 Speaker 1: are around right now? Some of the most of the 694 00:35:28,000 --> 00:35:29,719 Speaker 1: ones that are really big are going to be the 695 00:35:29,760 --> 00:35:31,839 Speaker 1: ones that are about to die because they're in this 696 00:35:31,960 --> 00:35:34,920 Speaker 1: last stage where they're blowing themselves up before they collapse. 697 00:35:35,400 --> 00:35:37,919 Speaker 1: Mm hmmm. Al right, well, let's go down the list. 698 00:35:37,920 --> 00:35:39,920 Speaker 1: What are some of the ones that are huge, you know, 699 00:35:39,960 --> 00:35:41,759 Speaker 1: just to get a sense of scale. There's a star, 700 00:35:41,840 --> 00:35:45,120 Speaker 1: for example, called gay Crux, which is like the nearest 701 00:35:45,280 --> 00:35:48,520 Speaker 1: giant star to the Sun, and it's got only one 702 00:35:48,560 --> 00:35:51,000 Speaker 1: and a half times the mass the Sun, but the 703 00:35:51,120 --> 00:35:54,800 Speaker 1: radius of this thing is a hundred and twenty times 704 00:35:54,840 --> 00:35:58,720 Speaker 1: the radius of the Sun, which makes it much much bigger. 705 00:35:59,640 --> 00:36:02,319 Speaker 1: And is it a start one point five times the 706 00:36:02,320 --> 00:36:04,480 Speaker 1: massive arson it's it's a pretty similar kind of star. 707 00:36:04,560 --> 00:36:07,279 Speaker 1: Then it's a pretty similar kind of star exactly. And 708 00:36:07,320 --> 00:36:10,080 Speaker 1: it's in the Southern Cross actually, so it's sort of famous. 709 00:36:10,160 --> 00:36:12,080 Speaker 1: But you know, it's much bigger. It's only got like 710 00:36:12,200 --> 00:36:15,200 Speaker 1: another fifty percent of the mass, but the volume is 711 00:36:15,239 --> 00:36:20,080 Speaker 1: like ten thousand times bigger. M m. Yeah, that's huge. 712 00:36:20,640 --> 00:36:22,560 Speaker 1: But is it just because it's in a different stage 713 00:36:22,560 --> 00:36:24,879 Speaker 1: than our Sun? Because our son is gonna get that big, right, 714 00:36:25,160 --> 00:36:27,239 Speaker 1: our stage is also going to get that big. So yeah, 715 00:36:27,280 --> 00:36:29,520 Speaker 1: this one is, like all the ones on our Biggest 716 00:36:29,560 --> 00:36:32,040 Speaker 1: Stars list, is near the end of its life. Oh 717 00:36:32,080 --> 00:36:35,560 Speaker 1: I see that these are like peak peak size. Yeah, exactly. 718 00:36:35,840 --> 00:36:37,759 Speaker 1: This is when their stars are really reaching, like the 719 00:36:37,800 --> 00:36:39,560 Speaker 1: peak of their career, you know, when they are the 720 00:36:39,680 --> 00:36:42,279 Speaker 1: biggest they're ever going to be, right, And so the 721 00:36:42,280 --> 00:36:44,360 Speaker 1: one we can see right now is this one called 722 00:36:44,400 --> 00:36:47,319 Speaker 1: gay Crux, which is a hundred times the size of 723 00:36:47,360 --> 00:36:49,920 Speaker 1: our son. That's huge. Yeah. It's radius is about a 724 00:36:50,000 --> 00:36:53,040 Speaker 1: hundred times, right, which means the volume is a hundred 725 00:36:53,080 --> 00:36:56,520 Speaker 1: cubed right, right, So it's huge. Arson was sitting next 726 00:36:56,560 --> 00:36:59,960 Speaker 1: to it, it would look like one percent. That's big, yeah, exactly. 727 00:37:00,160 --> 00:37:02,760 Speaker 1: The ratio between the Earth and our Sun is about 728 00:37:02,760 --> 00:37:05,520 Speaker 1: the same as our sun and this star, So this 729 00:37:05,560 --> 00:37:08,719 Speaker 1: thing is just enormous alright. So you can see that 730 00:37:08,760 --> 00:37:10,799 Speaker 1: in the nice sky. If you go out at nine 731 00:37:10,840 --> 00:37:12,880 Speaker 1: and look up, you can see this, yeah, exactly. If 732 00:37:12,920 --> 00:37:14,480 Speaker 1: you're in the southern hemisphere and you can see the 733 00:37:14,480 --> 00:37:17,399 Speaker 1: Southern Cross, then yes, you can see this enormous star. 734 00:37:18,120 --> 00:37:19,919 Speaker 1: All right. Well, what's the next one on the list? 735 00:37:20,040 --> 00:37:22,640 Speaker 1: Next one on the list is the Pistol Star. This 736 00:37:22,719 --> 00:37:26,520 Speaker 1: one is twenty five times the mass the really substantially bigger, 737 00:37:26,640 --> 00:37:30,000 Speaker 1: but it's got three hundred times the radius, right, And 738 00:37:30,040 --> 00:37:33,279 Speaker 1: remember the volume goes up by radius cubed, so you 739 00:37:33,440 --> 00:37:36,160 Speaker 1: double the radius, you're going up in volume by a 740 00:37:36,239 --> 00:37:39,239 Speaker 1: factor eight. And so this one's like three times the 741 00:37:39,360 --> 00:37:42,360 Speaker 1: radius of gack Rux, which means it's like almost thirty 742 00:37:42,440 --> 00:37:45,840 Speaker 1: times the volume of that previous star. Wow, at that size, 743 00:37:45,840 --> 00:37:48,480 Speaker 1: would that fit, for example, in our solar system or 744 00:37:48,520 --> 00:37:50,680 Speaker 1: would it take up the whole solar system? That would 745 00:37:50,719 --> 00:37:53,560 Speaker 1: not fit in our solar system very comfortably, right, it 746 00:37:53,600 --> 00:37:56,239 Speaker 1: would go out past the radius of the Earth. I 747 00:37:56,239 --> 00:37:59,000 Speaker 1: think Jupiter Saturn would still survive, but it would not 748 00:37:59,040 --> 00:38:00,600 Speaker 1: be good for us, Like, you would not want to 749 00:38:00,600 --> 00:38:04,919 Speaker 1: put this star in our solar system. Too big, it's 750 00:38:04,960 --> 00:38:07,719 Speaker 1: too big. And you can't even see this star by 751 00:38:07,760 --> 00:38:11,400 Speaker 1: e super big. It's super bright, but it's actually close 752 00:38:11,440 --> 00:38:13,560 Speaker 1: to the center of the galaxy where there's a lot 753 00:38:13,640 --> 00:38:16,320 Speaker 1: of gas and dust going on, so you can't actually 754 00:38:16,360 --> 00:38:19,359 Speaker 1: see it with the naked eye. It's hidden. Yeah, it's 755 00:38:19,400 --> 00:38:22,279 Speaker 1: hidden from us by all this interstellar dust. And what 756 00:38:22,480 --> 00:38:24,839 Speaker 1: to call it? Blue hyper giant? What does that mean? Well, 757 00:38:24,880 --> 00:38:27,720 Speaker 1: blue just tells you the kind of light that it's emitting, 758 00:38:28,120 --> 00:38:30,360 Speaker 1: and a hypergiant is just the stage of life that 759 00:38:30,400 --> 00:38:32,440 Speaker 1: it's in. All these stars when they're done with the 760 00:38:32,480 --> 00:38:34,920 Speaker 1: main sequence and they're about to blow themselves out. They 761 00:38:35,000 --> 00:38:38,880 Speaker 1: become giants or supergiants or hypergiants, depending on you know, 762 00:38:38,920 --> 00:38:42,040 Speaker 1: the radius. All right, well, what else do we know 763 00:38:42,200 --> 00:38:44,799 Speaker 1: is out there? What's the next biggest star? The next 764 00:38:44,840 --> 00:38:48,439 Speaker 1: one is Roe Cassiopeia. It's a yellow hypergiant. This one 765 00:38:48,520 --> 00:38:52,120 Speaker 1: is five hundred times the radius of the Sun. Wow. 766 00:38:52,719 --> 00:38:55,120 Speaker 1: So this is kind of what would happen to our star. 767 00:38:55,840 --> 00:38:58,279 Speaker 1: But like a little bigger star, eventually it would grow 768 00:38:58,280 --> 00:39:00,800 Speaker 1: to this big. This one is forty times the mass 769 00:39:00,840 --> 00:39:03,000 Speaker 1: of our Sun. Our star is never gonna get this big. 770 00:39:03,040 --> 00:39:05,799 Speaker 1: And because it's so massive, it also makes it more rare. Like, 771 00:39:05,840 --> 00:39:08,760 Speaker 1: we don't know very many of these yellow hyper giant 772 00:39:08,840 --> 00:39:11,600 Speaker 1: stars in the whole galaxy. The only like fifteen of 773 00:39:11,640 --> 00:39:14,120 Speaker 1: them that have ever been seen. Wow. And this one 774 00:39:14,280 --> 00:39:17,320 Speaker 1: is definitely bigger than our solar system. This one would 775 00:39:17,320 --> 00:39:21,040 Speaker 1: definitely like eat Earth and Mars, but actually wouldn't even 776 00:39:21,080 --> 00:39:23,919 Speaker 1: get out to Jupiter. Jupiter is much further out than 777 00:39:24,040 --> 00:39:26,720 Speaker 1: all the other planets because the asteroid belt in between. 778 00:39:28,080 --> 00:39:31,279 Speaker 1: But still that's huge, right, It's huge. I mean, that's 779 00:39:31,360 --> 00:39:34,279 Speaker 1: it's like fire front of times the radis of our Sun. Yeah. 780 00:39:34,320 --> 00:39:36,440 Speaker 1: I mean, if you look at the Solar system, for example, 781 00:39:36,680 --> 00:39:39,080 Speaker 1: zoomed out so you can see all the planets. Even 782 00:39:39,120 --> 00:39:42,319 Speaker 1: the huge Sun looks really really small. Now replace that 783 00:39:42,320 --> 00:39:45,239 Speaker 1: with an enormous star that's like the size of the 784 00:39:45,360 --> 00:39:48,640 Speaker 1: radius of Mars. The whole Solar system would look totally different, 785 00:39:48,880 --> 00:39:51,719 Speaker 1: right right, And from here on Earth, our Sun was 786 00:39:51,760 --> 00:39:53,560 Speaker 1: five hundred times bigger, you know, we would see it 787 00:39:53,640 --> 00:39:56,600 Speaker 1: take up the entire sky and then eventually eat does up. Yeah, 788 00:39:56,680 --> 00:39:59,440 Speaker 1: that would be really crazy. Imagine living on a planet 789 00:39:59,440 --> 00:40:05,440 Speaker 1: where the Sun took up the entire sky toast all right, Now, 790 00:40:05,480 --> 00:40:07,720 Speaker 1: what's the next biggest star that we can see? Next? 791 00:40:07,800 --> 00:40:10,800 Speaker 1: Is one that's pretty famous. It's actually Beetle Juice. Beetle 792 00:40:10,880 --> 00:40:14,400 Speaker 1: Juice is about a thousand times the radius of the Sun. Like, 793 00:40:14,520 --> 00:40:18,319 Speaker 1: it just totally dwarfs our entire solar system. This one 794 00:40:18,480 --> 00:40:20,320 Speaker 1: would even eat of Jupiter if you put it in 795 00:40:20,360 --> 00:40:23,400 Speaker 1: the center of the solar system. Interesting, And so again 796 00:40:23,440 --> 00:40:25,359 Speaker 1: it's a star that's kind of at its peak. It's 797 00:40:25,360 --> 00:40:27,720 Speaker 1: like it's burning really brightly right now. Yeah, And actually 798 00:40:27,719 --> 00:40:31,000 Speaker 1: this one is quite interesting recently because it's been dimming. 799 00:40:31,400 --> 00:40:34,000 Speaker 1: Like remember, Beetle Juice got dim all of a sudden 800 00:40:34,000 --> 00:40:36,279 Speaker 1: in a way nobody understood, and people thought, it is 801 00:40:36,360 --> 00:40:38,960 Speaker 1: gonna go supernova? Is it about to blow? And then 802 00:40:39,000 --> 00:40:41,160 Speaker 1: people thought, maybe it's just a big blob of dust 803 00:40:41,200 --> 00:40:43,239 Speaker 1: the past in front of beetle Juice, and other people thought, 804 00:40:43,480 --> 00:40:46,880 Speaker 1: maybe it's an alien superstructure. We really didn't understand it. 805 00:40:46,960 --> 00:40:49,520 Speaker 1: Maybe this is like a variable star that's like compressing 806 00:40:49,560 --> 00:40:52,719 Speaker 1: and then glowing, compressing and glowing. We didn't really understand it. 807 00:40:52,760 --> 00:40:56,920 Speaker 1: But this is definitely a much bigger star than our son. Wow, 808 00:40:56,960 --> 00:41:00,560 Speaker 1: a thousand times the size for Sun that would be huge. Yeah, 809 00:41:00,600 --> 00:41:02,600 Speaker 1: if you're sitting in front of it. Yeah, and so 810 00:41:02,920 --> 00:41:05,959 Speaker 1: a thousand times the radius of the Sun, right means 811 00:41:06,000 --> 00:41:09,319 Speaker 1: a thousand cubed of the volume, And so that's a 812 00:41:09,400 --> 00:41:12,640 Speaker 1: billion times the volume of the Sun. Remember, TI was like, 813 00:41:12,680 --> 00:41:14,239 Speaker 1: I wonder if there are stars out there that are 814 00:41:14,239 --> 00:41:16,560 Speaker 1: like a million times the volume of the Sun. We're like, 815 00:41:16,640 --> 00:41:20,040 Speaker 1: here's one that fits a billion sons inside of it. Yeah, 816 00:41:20,080 --> 00:41:21,919 Speaker 1: that's that's why. Well, I hope we blew your mind. 817 00:41:21,960 --> 00:41:25,239 Speaker 1: Tie all right, So then let's maybe skip a little 818 00:41:25,239 --> 00:41:27,040 Speaker 1: bit ahead to what is the biggest star that we 819 00:41:27,080 --> 00:41:29,080 Speaker 1: know about, like in terms of size that you can 820 00:41:29,080 --> 00:41:30,960 Speaker 1: see in the night sky. What is the biggest one 821 00:41:30,960 --> 00:41:33,560 Speaker 1: that you can see, the biggest one out there right now. 822 00:41:33,600 --> 00:41:38,600 Speaker 1: The current champion is one called Stevenson to eighteen. This 823 00:41:38,640 --> 00:41:42,160 Speaker 1: one has more than two thousand times the radius of 824 00:41:42,200 --> 00:41:47,560 Speaker 1: our sun. Wow, two thousand times bigger, which means it's like, 825 00:41:47,680 --> 00:41:50,840 Speaker 1: you know, a bazillion times more volume. It's yeah, exactly, 826 00:41:50,880 --> 00:41:55,240 Speaker 1: It's like more than sixteen billion sons could fit inside 827 00:41:55,239 --> 00:41:58,000 Speaker 1: this thing. If you dropped the sun into this thing, 828 00:41:58,040 --> 00:42:00,840 Speaker 1: you wouldn't even notice it. Wow. And how much brighter 829 00:42:00,920 --> 00:42:04,120 Speaker 1: is it? It's a half million times brighter. So you 830 00:42:04,200 --> 00:42:07,000 Speaker 1: put half a million sons together and you get the 831 00:42:07,000 --> 00:42:10,400 Speaker 1: brightness of this thing. Five thousand sons in one place. 832 00:42:10,560 --> 00:42:13,600 Speaker 1: That's crazy in one place. Yeah, it's just it's taking 833 00:42:13,719 --> 00:42:16,319 Speaker 1: up so much space. It's incredible. Like if you try 834 00:42:16,400 --> 00:42:19,640 Speaker 1: to fly around this thing in a spaceship, it would 835 00:42:19,680 --> 00:42:23,000 Speaker 1: take you like nine hours at light speed just to 836 00:42:23,080 --> 00:42:26,680 Speaker 1: do one orbit around this star. Wow, that's crazy. It 837 00:42:26,719 --> 00:42:30,360 Speaker 1: takes hours for the light just to leave this star exactly. 838 00:42:30,640 --> 00:42:33,000 Speaker 1: If you're a photon generated at the heart of this thing, 839 00:42:33,239 --> 00:42:36,239 Speaker 1: you're not getting out there for a while, all right. 840 00:42:36,280 --> 00:42:38,200 Speaker 1: So that's that is the biggest star that we can see. 841 00:42:38,200 --> 00:42:41,760 Speaker 1: It's thousands of times bigger than our sun. Bazillion times 842 00:42:41,960 --> 00:42:45,960 Speaker 1: bazillion is at the technical term bigger and volume than 843 00:42:46,120 --> 00:42:49,359 Speaker 1: our star, and it's half a million times brighter. It's 844 00:42:49,440 --> 00:42:52,520 Speaker 1: really impressive. It definitely deserves some kind of prize. And 845 00:42:52,760 --> 00:42:54,560 Speaker 1: you can see it in the night sky. Is out 846 00:42:54,600 --> 00:42:56,959 Speaker 1: there in the night sky. It's near this cluster called 847 00:42:57,000 --> 00:42:59,840 Speaker 1: Stephenson two, which is why it's called Stevenson two eighteen. 848 00:43:00,239 --> 00:43:02,640 Speaker 1: And you can't see it by eyes. Actually discovered in 849 00:43:02,680 --> 00:43:08,360 Speaker 1: around by astronomers using infrared telescopes. Wow, that's wild. That's huge. 850 00:43:08,680 --> 00:43:11,359 Speaker 1: So you can't see it because it's so far away. Yeah, 851 00:43:11,400 --> 00:43:14,359 Speaker 1: this thing is like twenty thousand light years from Earth. 852 00:43:14,560 --> 00:43:16,920 Speaker 1: So remember the brightness of a star falls with like 853 00:43:16,960 --> 00:43:20,320 Speaker 1: the distance squared, and so if you're twice as far away, 854 00:43:20,600 --> 00:43:22,799 Speaker 1: it's a quarter of the brightness. And so this one, 855 00:43:22,800 --> 00:43:25,920 Speaker 1: we're twenty thousand light years away, which is why it's 856 00:43:25,960 --> 00:43:29,439 Speaker 1: apparently so dim to the naked eye. But I guess 857 00:43:29,440 --> 00:43:31,279 Speaker 1: if you have a telescope, you can see it and 858 00:43:31,320 --> 00:43:33,320 Speaker 1: you can sort of model its size. You can model 859 00:43:33,320 --> 00:43:36,239 Speaker 1: its size by understanding its luminosity and its temperature, and 860 00:43:36,280 --> 00:43:38,560 Speaker 1: then we can do these calculations but we definitely can't 861 00:43:38,600 --> 00:43:41,920 Speaker 1: measure directly, and that's a shame, because man, I would 862 00:43:41,920 --> 00:43:44,120 Speaker 1: love to see this thing close up, Like, what is 863 00:43:44,160 --> 00:43:46,919 Speaker 1: the surface of this thing look like? Yeah, what would 864 00:43:46,920 --> 00:43:48,640 Speaker 1: it look like? Is it a different color or is 865 00:43:48,680 --> 00:43:51,080 Speaker 1: it just a big bright yellow ball. Well, it's a 866 00:43:51,160 --> 00:43:54,480 Speaker 1: red super giant, so probably would be mostly red. But yeah, 867 00:43:54,560 --> 00:43:56,399 Speaker 1: you know, if you look at pictures of the sun 868 00:43:56,440 --> 00:43:57,880 Speaker 1: close up, you notice that there are a lot of 869 00:43:57,880 --> 00:44:00,160 Speaker 1: like hot spots and cold spots. It's like a lot 870 00:44:00,160 --> 00:44:02,279 Speaker 1: of stuff going on. So I think you'd see the 871 00:44:02,320 --> 00:44:04,439 Speaker 1: same thing. But we've never seen one of these things 872 00:44:04,440 --> 00:44:07,279 Speaker 1: super close up. It would be an awesome opportunity to 873 00:44:07,400 --> 00:44:09,640 Speaker 1: learn more about how a star gets really big and 874 00:44:09,640 --> 00:44:11,120 Speaker 1: what it looks like at the end of its life 875 00:44:11,120 --> 00:44:14,200 Speaker 1: cycle if we could. But you know, it's so far away, right, 876 00:44:14,280 --> 00:44:16,120 Speaker 1: And what kind of star is this? Is it like 877 00:44:16,200 --> 00:44:18,759 Speaker 1: our star but you put more hydrogen into it or 878 00:44:18,800 --> 00:44:21,400 Speaker 1: is it something fundamentally different. No, it's just like a 879 00:44:21,440 --> 00:44:23,759 Speaker 1: bigger serving of hydrogen. It's just got a lot more 880 00:44:23,840 --> 00:44:25,760 Speaker 1: mass than our star. Like, we don't have a precise 881 00:44:25,840 --> 00:44:28,560 Speaker 1: number for how much mass it has. It's not always 882 00:44:28,560 --> 00:44:31,600 Speaker 1: easy to measure for these really really big, very bright stars. 883 00:44:32,320 --> 00:44:34,560 Speaker 1: But it just started out with a bigger helping and 884 00:44:34,600 --> 00:44:36,920 Speaker 1: that's why I ended up a much bigger star. And 885 00:44:36,960 --> 00:44:38,719 Speaker 1: then you wait sort of for the end of its 886 00:44:38,760 --> 00:44:41,440 Speaker 1: life cycle. It's like a really massive star also at 887 00:44:41,440 --> 00:44:44,799 Speaker 1: the peak of its size. Wow, it's hot stuff. It's 888 00:44:44,880 --> 00:44:50,120 Speaker 1: hot stuff, exactly alright. So we covered the most voluminous 889 00:44:50,160 --> 00:44:53,160 Speaker 1: star and also the most massive star. So the most 890 00:44:53,160 --> 00:44:57,680 Speaker 1: massive star is our one three six A one, which 891 00:44:57,960 --> 00:45:01,160 Speaker 1: is two hundred times the massive our Sun, and the 892 00:45:01,200 --> 00:45:04,960 Speaker 1: most voluminous the biggest star is about two thousand times 893 00:45:04,960 --> 00:45:07,640 Speaker 1: the size war Sun. Yeah, two thousand times of radius 894 00:45:07,680 --> 00:45:10,680 Speaker 1: and then billions of times the volume, all right, and 895 00:45:10,880 --> 00:45:13,520 Speaker 1: that basically makes me feel small, Daniel. That was the 896 00:45:13,560 --> 00:45:16,200 Speaker 1: goal of the podcast exactly to think about the size 897 00:45:16,200 --> 00:45:17,920 Speaker 1: of the stuff that's out there in the universe. And 898 00:45:18,040 --> 00:45:22,799 Speaker 1: remember that we're pretty tiny compared to the enormous, powerful 899 00:45:22,880 --> 00:45:26,480 Speaker 1: forces creating these objects out there. Yeah, because they make 900 00:45:26,520 --> 00:45:29,680 Speaker 1: our star look tiny, and we're super tiny compared to 901 00:45:29,680 --> 00:45:32,360 Speaker 1: our Sun. Yeah, we're even super tiny compared to our Earth, 902 00:45:32,680 --> 00:45:35,200 Speaker 1: which is super tiny compared to our Sun, which turns 903 00:45:35,239 --> 00:45:37,239 Speaker 1: out to be a pip squeak in the universe. Well, 904 00:45:37,239 --> 00:45:39,080 Speaker 1: It's pretty amazing to sort of think about, because the 905 00:45:39,120 --> 00:45:41,160 Speaker 1: recipe for all these stars is the same. You know, 906 00:45:41,239 --> 00:45:43,520 Speaker 1: it's just ad hydrogen, but you know, you get all 907 00:45:43,560 --> 00:45:46,799 Speaker 1: this huge variation in like what's happening in the processes 908 00:45:46,840 --> 00:45:50,560 Speaker 1: and the volume and the mass. It's a pretty complex 909 00:45:50,760 --> 00:45:53,520 Speaker 1: and impressive universe. Yeah. I do like the idea of 910 00:45:53,520 --> 00:45:56,239 Speaker 1: a star having a recipe which is one ingredient and 911 00:45:56,280 --> 00:46:01,960 Speaker 1: one step right, but no more right, Like, if you 912 00:46:02,000 --> 00:46:03,799 Speaker 1: get it off by a little bit, it becomes a 913 00:46:03,840 --> 00:46:05,799 Speaker 1: totally different star. That's true. If you get it off 914 00:46:05,800 --> 00:46:08,000 Speaker 1: by a factor of five hundred, then you no longer 915 00:46:08,040 --> 00:46:10,040 Speaker 1: get a star. But that's also true of cookies. You know, 916 00:46:10,120 --> 00:46:12,319 Speaker 1: you put in five times too much sugar, they're not 917 00:46:12,360 --> 00:46:15,720 Speaker 1: really cookies anymore, right, Or five hundred times more chocolate chips, 918 00:46:16,480 --> 00:46:19,200 Speaker 1: you just get a chocolate chip exactly. That's just a 919 00:46:19,239 --> 00:46:21,160 Speaker 1: recipe for a chocolate chip. It sounds like a star 920 00:46:21,200 --> 00:46:23,879 Speaker 1: of a recipe. I have strong opinions, but I would 921 00:46:23,880 --> 00:46:28,919 Speaker 1: taste it. You would just taste chocolate. It's like, oh, yeah, 922 00:46:28,960 --> 00:46:31,680 Speaker 1: that's an interesting recipe. Chunk of chocolate with little tiny 923 00:46:31,760 --> 00:46:35,520 Speaker 1: cookies ambitted in it. A cookie chip. Yeah, all right, Well, 924 00:46:35,680 --> 00:46:37,560 Speaker 1: We hope you enjoyed that and made you think about 925 00:46:37,800 --> 00:46:40,880 Speaker 1: the brightness and the amazing things that are shining out 926 00:46:40,960 --> 00:46:43,920 Speaker 1: during the night sky. And remember that however big you 927 00:46:43,960 --> 00:46:46,960 Speaker 1: think things are, they're actually much more vast than you 928 00:46:46,960 --> 00:46:49,960 Speaker 1: could ever possibly imagine. All Right, we hope you enjoyed that. 929 00:46:50,200 --> 00:47:00,840 Speaker 1: Thanks for joining us, see you next time. Thanks for listening, 930 00:47:00,840 --> 00:47:03,560 Speaker 1: and remember that Daniel and Jorge Explain the Universe is 931 00:47:03,600 --> 00:47:07,080 Speaker 1: a production of I Heart Radio. Or more podcast from 932 00:47:07,120 --> 00:47:10,879 Speaker 1: my heart Radio visit the I heart Radio app, Apple Podcasts, 933 00:47:11,000 --> 00:47:14,320 Speaker 1: or wherever you listen to your favorite shows. H