What Happens If A Star Explodes Near The Earth?
Veritasium | November 15, 2022
Posted on 11/24/2022 2:29:38 PM PST by SunkenCiv
What Happens If A Star Explodes Near The Earth?
Veritasium | November 15, 2022
(Excerpt) Read more at youtube.com ...
Flood, Fire, and Famine
in the History of Civilization
by Richard Firestone,
Allen West, and
Simon Warwick-Smith
It will take a long time to clean up
I think Rosie O’Donnell blew up once. It wasn’t pretty.
Better a star than Uranus.
Duct tape, Bondo, beer, and hot babes required for clean up
How big is the star? How far away is the star? Inverse square law is our friend.
Is this more severe than Brittany Spears in 2007?
Iirc the closest star is like 4.3 light years away.
all the rest of them are much further.
so if you take squares of difference and energy released into account any random average star exploding would have less effect on earth than a typical politician.
If it is Sirius, 16 light years away, then we have a problem. If it is Betelgeuse, 300 light years away, we have a spectacular light show.
300 miles away? I thought Betelgeuse was in Chicago?
Like the one 93 million miles away?
âïļðð
Stupid Sarah sees a face!
ðĪŠð
well, if it’s our star/sun, problems are over...
Some related keywords, sorted, edited (a bunch of chaff, plus APOD topics removed):
Nice job, workin’ that in. :^)
Some of those will buff right out.
| Transcript | |
| 0:00 | - What would happen if |
| 0:01 | a star exploded near the earth? |
| 0:04 | Well, the nearest star to Earth, of course, is the sun, |
| 0:07 | and it is not going to explode, |
| 0:09 | but if it had eight times the mass, |
| 0:12 | then it would go supernova at the end of its life. |
| 0:15 | So what would that look like? |
| 0:17 | Well, as noted by xkcd if you held up |
| 0:20 | a hydrogen bomb right to your eyeball and detonated it, |
| 0:25 | that explosion would still be a billion times less bright |
| 0:30 | than watching the sun go supernova from Earth. |
| 0:36 | That's how insanely powerful supernova explosions are. |
| 0:39 | They are the biggest explosions in the universe. |
| 0:42 | When we see supernovae in other galaxies, |
| 0:45 | they are brighter than the combined light |
| 0:48 | of hundreds of billions of stars, so bright, in fact, |
| 0:52 | that they appear to come out of nowhere. |
| 0:55 | On the 8th of October, 1604, |
| 0:57 | the astronomer Johannes Kepler looked up into the night sky |
| 1:01 | and noticed a bright star he had never seen before. |
| 1:05 | It was brighter than all the other stars in the sky |
| 1:08 | and about as bright as the planet Jupiter. |
| 1:12 | On moonless nights, it was bright enough to cast a shadow. |
| 1:16 | Kepler published his observations |
| 1:18 | of this star in a book called "De Stella Nova," |
| 1:20 | which means "about a new star" in Latin. |
| 1:24 | Kepler thought he was witnessing the birth of a new star, |
| 1:28 | but it was actually a star's violent death. |
| 1:32 | Over the following year and a half, |
| 1:33 | the light faded until it was no longer visible, |
| 1:37 | but the name stuck. |
| 1:39 | Even once we learned what was really happening in the 1930s, |
| 1:42 | the violent final explosion for stars |
| 1:45 | between about 8 and 30 solar masses |
| 1:47 | has been called a supernova. |
| 1:51 | But how exactly a star explodes is not |
| 1:54 | what most people think. |
| 1:57 | For most of a star's life, it exists in a stable balance. |
| 2:00 | In its core, it fuses lighter elements together |
| 2:03 | to make heavier ones, and in the process |
| 2:05 | it converts a small amount of matter into energy. |
| 2:08 | This energy is really what keeps the star |
| 2:11 | from collapsing in on itself. |
| 2:14 | Gravity compresses the star, |
| 2:16 | but that force is counteracted by the pressure generated |
| 2:19 | by the movement of particles inside the star, |
| 2:22 | and by the pressure of photons released by fusion. |
| 2:26 | So in effect, stars are propped up by their own light. |
| 2:32 | If the rate of fusion drops at the center of the star, |
| 2:34 | the temperature and the pressure decrease. |
| 2:37 | Gravity starts winning, compressing the star, |
| 2:41 | but this increases the temperature and pressure in the core, |
| 2:44 | which increases the rate of fusion. |
| 2:46 | It's a stable self-regulating system, but there's a problem. |
| 2:51 | Stars have a finite amount of fuel, |
| 2:54 | which over time gets used up. |
| 2:56 | Our sun is about 5 billion years |
| 2:59 | into its 10-billion-year lifespan. |
| 3:02 | There are stars dozens of times more massive than the sun, |
| 3:05 | which you would think would live much longer, |
| 3:07 | but they actually use up their nuclear fuel faster |
| 3:11 | A star 20 times the mass of our sun has |
| 3:13 | a lifespan of just 10 million years, |
| 3:16 | and more massive stars burn hotter, and even brighter, |
| 3:20 | but for much shorter lives. |
| 3:22 | For 90% the life of a star, |
| 3:24 | the core is only hot enough to fuse hydrogen into helium, |
| 3:29 | and when the hydrogen runs out, |
| 3:31 | fusion slows, gravity compresses the core |
| 3:34 | and its temperature increases to 200 million degrees, |
| 3:38 | at which point helium fuses into carbon. |
| 3:41 | There's enough helium to power the star for around |
| 3:44 | a million years, but as the helium runs out, |
| 3:47 | the core is, again, compressed and heated. |
| 3:49 | Carbon starts fusing into neon, |
| 3:51 | which lasts about 1,000 years, |
| 3:53 | and then neon fuses into oxygen for a few more years, |
| 3:57 | then oxygen to silicon for a few months |
| 4:00 | and at 2.5 billion degrees, silicon fuses |
| 4:03 | into nickel which decays into iron. |
| 4:07 | Now, at the heart of this giant star, |
| 4:08 | there is an iron core building that's only |
| 4:12 | a few thousand kilometers across. |
| 4:15 | Iron is where this pattern stops. |
| 4:17 | Instead of liberating energy as it fuses |
| 4:20 | into heavier elements, it actually requires energy. |
| 4:24 | Iron is the most stable element. |
| 4:27 | So it actually takes energy both |
| 4:28 | to fuse it into heavier elements |
| 4:30 | and to break it down into lighter ones. |
| 4:33 | Both fusion and fission reactions ultimately end up at iron. |
| 4:38 | The iron core grows, |
| 4:40 | but the crush of gravity becomes greater |
| 4:42 | and greater as the rate of fusion drops. |
| 4:45 | When the iron core is about 1.4 times the mass of our sun, |
| 4:49 | which is known as the Chandrasekhar limit, the pull |
| 4:52 | of gravity is so strong that something totally wild happens. |
| 4:56 | Quantum mechanics takes over. |
| 4:58 | Electrons run out of room to move, |
| 5:01 | and they're forced into their lowest energy states, |
| 5:04 | and they then become absorbed by the protons in the nucleus. |
| 5:09 | In this process, the protons turn |
| 5:11 | into neutrons and release neutrinos. |
| 5:15 | With the electrons gone, the core collapses, |
| 5:18 | and fast, at about 25% the speed of light. |
| 5:22 | So what used to be a ball |
| 5:23 | of iron 3,000 kilometers in diameter becomes |
| 5:27 | a ball of neutrons just 30 kilometers across. |
| 5:30 | Essentially, it's a neutron star. |
| 5:33 | With no outward pressure to hold it up, |
| 5:36 | the rest of the star caves in. |
| 5:38 | Also, falling at a quarter of the speed of flight, |
| 5:41 | it hits the neutron star and bounces off, |
| 5:44 | creating a huge pressure wave. |
| 5:46 | But this kinetic energy isn't quite enough |
| 5:49 | to start a supernova explosion. |
| 5:51 | No, the thing that really kicks it off |
| 5:53 | is the humble neutrino. |
| 5:55 | Now, I normally think of neutrinos |
| 5:57 | as particles that do basically nothing. |
| 6:00 | I mean, they interact so rarely with matter |
| 6:02 | that right now there are 100 trillion neutrinos |
| 6:05 | passing through your body per second. |
| 6:08 | It would take a light year of lead just |
| 6:10 | to give you a 50-50 chance of stopping a neutrino, |
| 6:14 | and that's because they interact only |
| 6:15 | through gravity and the weak force |
| 6:18 | but in a supernova, when the electrons are captured |
| 6:21 | by the protons, an unbelievable number |
| 6:23 | of neutrinos is released, around 10^58. |
| 6:28 | You would think they would just fly off |
| 6:30 | at nearly the speed of light, but the core |
| 6:33 | of a supernova is incredibly dense, |
| 6:35 | about 10 trillion times more dense than lead |
| 6:39 | and as a result, it traps some of those neutrinos |
| 6:43 | and captures their energy, |
| 6:45 | and this is what makes a star go supernova. |
| 6:48 | A particle that is millions |
| 6:50 | of times less massive than an electron that barely interacts |
| 6:54 | with anything is responsible for some |
| 6:57 | of the largest explosions in the universe. |
| 7:01 | In that explosion, only 1/100 of 1% |
| 7:05 | of the energy is released as electromagnetic radiation, |
| 7:08 | the light that we can see. |
| 7:10 | Even then, supernova have enough energy |
| 7:12 | to outshine a whole galaxy. |
| 7:14 | About 1% of the energy is released as the kinetic energy |
| 7:18 | of the exploding matter, but the vast majority |
| 7:21 | of the energy is released in the form |
| 7:24 | of neutrinos, and neutrinos are actually |
| 7:27 | the first signal we detect from supernovae, |
| 7:31 | and that's because after they're generated |
| 7:33 | in the core, they can escape |
| 7:36 | before the shockwave reaches the surface, |
| 7:38 | where the light that we see is generated. |
| 7:41 | So neutrinos can arrive on Earth hours before the photons, |
| 7:44 | giving astronomers a chance to aim their telescopes |
| 7:47 | at the right part of the sky. |
| 7:51 | I actually used to work |
| 7:52 | at a neutrino observatory back in college, |
| 7:54 | and I would work the graveyard shift |
| 7:56 | between midnight and 8:00 AM. |
| 7:58 | So if I detected a really big increase |
| 8:01 | in the neutrino flux during my shift, |
| 8:02 | it was my job to call and wake up scientists, |
| 8:06 | so they could go look out for a supernova. |
| 8:09 | Now, that never actually happened, |
| 8:10 | but we did have some close calls. |
| 8:12 | Now, I need to clarify a couple things. |
| 8:15 | First, not all really massive stars explode. |
| 8:18 | As they collapse, some form black holes instead, |
| 8:21 | which means they do not go supernova |
| 8:24 | and second, there's another way to make a supernova. |
| 8:27 | Sometimes a white dwarf star, which is incredibly dense, |
| 8:30 | pulls matter off a nearby star, and when it's mass reaches |
| 8:34 | that Chandrasekhar limit of 1.4 solar masses, |
| 8:37 | the white dwarf collapses, creating a supernova. |
| 8:41 | This is actually the type of supernova that Kepler saw |
| 8:43 | in 1604, a supernova 20,000 light years from Earth. |
| 8:49 | Now, because the shocks are asymmetric, |
| 8:51 | supernova explain neutron stars that can move really fast. |
| 8:56 | There's a neutron star we've observed with a velocity |
| 8:58 | of 1,600 kilometers per second, and we think that was caused |
| 9:04 | by a very asymmetric supernova explosion, |
| 9:07 | sent it shooting off in the other direction. |
| 9:10 | Despite only recently learning about how supernovae work, |
| 9:13 | humans have been observing them for thousands of years. |
| 9:17 | Ancient Indian, Chinese, Arabic |
| 9:19 | and European astronomers all observed supernovae, |
| 9:23 | but they are quite rare. |
| 9:25 | In a galaxy like our Milky Way, |
| 9:27 | consisting of 100 billion stars, |
| 9:30 | there are only about one or two supernovae per century. |
| 9:34 | A particularly amazing example is the supernova of 1054, |
| 9:39 | when the light of a supernova 6,500 light years away |
| 9:42 | reached the earth and was recorded by Chinese astronomers. |
| 9:47 | If we look to where that supernova was recorded, |
| 9:50 | we see the Crab Nebula. |
| 9:52 | It is a giant remnant of radioactive matter, |
| 9:56 | left behind by the explosion. |
| 9:58 | In the 1,000 years since the explosion, |
| 10:01 | the remnant has grown to 11 light years in diameter. |
| 10:05 | Supernovas produce a lot of cosmic rays. |
| 10:08 | Cosmic rays are actually particles, |
| 10:10 | mainly protons and helium nuclei, |
| 10:13 | and they travel out at very, |
| 10:15 | very nearly the speed of light. |
| 10:17 | They have a tremendous amount of energy. |
| 10:20 | So at what distance could |
| 10:22 | a supernova cause problems for life on Earth? |
| 10:25 | The closest stars to us, besides the sun, |
| 10:27 | are the three stars in Alpha Centauri. |
| 10:30 | They are 4.4 light years away, but stars do move around |
| 10:35 | and on average, a star gets within one light year |
| 10:38 | of Earth every 500,000 years. |
| 10:41 | So what would happen if such a star went off? |
| 10:46 | - Yeah, so within a light year, you're easily |
| 10:48 | within a danger distance from just the kinetic energy. |
| 10:52 | So I think even at that distance, |
| 10:54 | you're looking at possibly blowing the atmosphere off. |
| 10:58 | - But we would also |
| 10:59 | have other problems to worry about. |
| 11:01 | Supernovae create conditions that are hot enough |
| 11:03 | to fuse elements heavier than iron. |
| 11:06 | In the months after the explosion, these elements |
| 11:09 | undergo radioactive decay, producing gamma rays |
| 11:12 | and cosmic rays. |
| 11:14 | Less than 0.1% of the energy produced |
| 11:16 | by a supernova is emitted as gamma rays |
| 11:19 | from these radioactive decays, |
| 11:20 | but even this tiny percentage can be dangerous. |
| 11:24 | At a few light years from a supernova, |
| 11:26 | the radiation could be deadly, though most |
| 11:29 | of it would be blocked by our atmosphere. |
| 11:33 | Now, the earth is protected from solar and cosmic radiation |
| 11:36 | by our atmosphere, and specifically by ozone molecules, |
| 11:41 | three oxygen atoms bonded together, |
| 11:43 | but high energy cosmic rays from supernova can come down |
| 11:47 | and break apart nitrogen molecules in the atmosphere, |
| 11:52 | and then these bond with oxygen atoms, |
| 11:55 | which can then break apart ozone, |
| 11:58 | and so we can lose a lot of our ozone |
| 12:01 | if there's too many cosmic rays coming |
| 12:03 | from supernova events, and that can expose us |
| 12:05 | to all kinds of dangerous radiation coming in from space. |
| 12:09 | We actually see an increase |
| 12:10 | in atmospheric NO3 concentrations, |
| 12:13 | coinciding with supernova explosions. |
| 12:16 | A supernova within 30 light years is rare, |
| 12:19 | only happening maybe once every 1 1/2 billion years or so, |
| 12:23 | but a recent article suggests supernovae could be lethal all |
| 12:26 | the way out to 150 light years away, |
| 12:30 | and so those would be much more common. |
| 12:32 | We actually have evidence |
| 12:34 | for a supernova that went off 150 light years |
| 12:36 | from Earth 2.6 million years ago. |
| 12:39 | It would've been seen by our early human ancestors, |
| 12:42 | like Australopithecus, and we know this |
| 12:45 | because there are elements present on Earth |
| 12:47 | that could only have been deposited by a recent supernova. |
| 12:51 | In sedimentary rocks at the bottom of the Pacific Ocean, |
| 12:54 | scientists have found traces of iron-60, |
| 12:57 | in a layer that was deposited 2.6 million years ago. |
| 13:02 | Iron-60 is an isotope of iron |
| 13:04 | with four more neutrons than the most common type of iron. |
| 13:08 | Iron-60 is really hard to make. |
| 13:10 | Our sun doesn't make it, nor is it produced, basically, |
| 13:13 | anywhere else in the solar system. |
| 13:15 | Iron-60 is made, basically, exclusively |
| 13:18 | in supernova explosions, |
| 13:20 | and iron-60 is radioactive. |
| 13:22 | It has a half life of 2.6 million years. |
| 13:25 | So every 2.6 million years, |
| 13:27 | half of the sample decays into cobalt-60. |
| 13:31 | So all of the iron-60 that was around during the formation |
| 13:34 | of the earth, 4.5 billion years ago, |
| 13:36 | has definitely decayed. |
| 13:38 | So the iron-60 that the scientists measure |
| 13:41 | is proof of a recent supernova. |
| 13:43 | Scientists also measured trace amounts of manganese-53 |
| 13:47 | in the same sediments, giving further evidence |
| 13:49 | supporting the idea that recently there was |
| 13:52 | an explosion of a nearby supernova. |
| 13:55 | The supernova that happened 2.6 million years ago |
| 13:58 | wasn't catastrophic for our ancestors, |
| 14:01 | but some researchers hypothesized that it could be related |
| 14:04 | to the mass extinction, which is seen |
| 14:05 | at the Pliocene-Pleistocene boundary |
| 14:08 | in the fossil record around the same time. |
| 14:11 | This extinction wiped out around 1/3 of marine megafauna. |
| 14:15 | The idea is that the cosmic rays |
| 14:17 | from the supernova hit particles in our atmosphere, |
| 14:20 | creating muons, which are charged particles |
| 14:23 | like the electron, only more than 200 times heavier. |
| 14:26 | The muon flux for years after the supernova |
| 14:29 | would've been 150 times higher than normal, |
| 14:33 | and the bigger the animal, the larger |
| 14:35 | the radiation dose it would've received from these muons, |
| 14:38 | which is why megafauna were so disproportionately affected, |
| 14:42 | and what's more, the animals that lived |
| 14:45 | in shallower waters were more likely |
| 14:47 | to become extinct compared to the ones that lived at depth, |
| 14:50 | where the water would've protected them from muons. |
| 14:54 | Further evidence for these recent nearby supernovae comes |
| 14:57 | from our place in the galaxy. |
| 15:00 | You know, if you look in the space |
| 15:01 | between the stars in our galaxy, on average, |
| 15:04 | there are around a million hydrogen atoms per cubic meter. |
| 15:08 | That may sound like a lot, |
| 15:09 | but it's basically a perfect vacuum |
| 15:11 | but for hundreds of light years |
| 15:14 | in all directions around our solar system, |
| 15:17 | you find there are 1,000 times fewer hydrogen atoms. |
| 15:21 | It's like they've all been blown out somewhere, |
| 15:24 | and our solar system is existing in this cosmic void, |
| 15:28 | inside a low density bubble. |
| 15:31 | So that is evidence for maybe tens of supernovae |
| 15:34 | that would've blown all this material outwards, |
| 15:38 | but there are cosmic explosions that are even |
| 15:40 | more deadly than normal supernovae, gamma ray bursts. |
| 15:44 | Gamma ray bursts were discovered by the Vela satellites, |
| 15:47 | which were looking for Soviet nuclear tests |
| 15:50 | but on the 2nd of July, 1967, |
| 15:52 | the satellites detected a large burst of gamma rays, |
| 15:56 | which were coming from space. |
| 15:59 | There are two main sources of gamma ray bursts, |
| 16:02 | mergers of neutron stars and the core collapses |
| 16:05 | of gigantic stars called hypernovae. |
| 16:08 | Hypernovae are caused by stars that are |
| 16:10 | at least 30 solar masses and rapidly spinning. |
| 16:14 | Their collapse leads to an explosion 10 times more powerful |
| 16:18 | than a regular supernova, and it leaves behind a black hole. |
| 16:23 | The gamma ray bursts caused by hypernovae channel most |
| 16:27 | of their energy into beams |
| 16:28 | which are just a few degrees across. |
| 16:32 | If there was a gamma ray burst within 6,000 light years, |
| 16:35 | it would decrease the ozone level enough |
| 16:38 | that it could be catastrophic. |
| 16:40 | To put this distance in context, a sphere with a radius |
| 16:43 | of 6,000 light years contains hundreds of millions of stars. |
| 16:49 | On October 9th, 2022, astronomers detected one |
| 16:52 | of the most powerful gamma ray bursts ever measured. |
| 16:55 | It was powerful enough to measurably affect how |
| 16:58 | the ionosphere bounces radio waves. |
| 17:00 | The effect on the ionosphere was |
| 17:02 | around the same as a solar flare, |
| 17:05 | but this gamma ray burst was located |
| 17:07 | in a galaxy 2.5 billion light years away. |
| 17:12 | Astronomers speculate that a gamma ray burst |
| 17:14 | could have caused the Late Ordovician mass extinction, |
| 17:17 | which wiped out 85% of marine species 440 million years ago. |
| 17:23 | There is no direct evidence, |
| 17:25 | but gamma ray bursts are common enough |
| 17:27 | that it is estimated that there has been |
| 17:29 | a 50% chance that there was |
| 17:31 | an ozone-removing, extinction-causing GRB |
| 17:34 | in the vicinity of Earth in the last 500 million years. |
| 17:38 | So if a supernova or a gamma ray burst were |
| 17:41 | to go off near the earth now, |
| 17:43 | that would be pretty catastrophic but in an ironic twist, |
| 17:47 | we kind of owe our existence to these sorts |
| 17:50 | of explosions because 4.6 billion years ago, |
| 17:54 | it was probably the shockwave from a nearby supernova |
| 17:58 | which triggered the collapse of a cloud of gas |
| 18:02 | and dust that gradually coalesced to form our solar system. |
| 18:06 | So the sun, the earth and all of us wouldn't be here today |
| 18:11 | without the explosions of nearby stars. |
| 18:22 | Figuring out how supernova explode was incredibly difficult. |
| 18:25 | It took a combination of astrophysics, |
| 18:27 | particle physics, computer science and mathematics, |
| 18:30 | and if you wanna develop a better understanding |
| 18:32 | of our universe, then you should check out |
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How many thousand lightyears is “close”?
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