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Can you please tell us about the newly found third type of supernova? You have been asking many questions from the past three sessions. I hope you are okay, so here we are. What is the so? Let'S first talk about the first two types of supernova there's the type one supernova and the type two supernovae. So let's talk about type two first, which is strange, but let's talk about that first uh.
So the type two supernovae is when you have a star. So first, let's talk about our own sun. Will our own sun go supernova? It won't. It is too small to undergo a supernova explosion, so our sun basically contains about 73 percent hydrogen 25 helium and then some other trace trace of other heavier elements and the nuclear energy I mean. The nuclear reaction within the sun is the fusion of hydrogen into helium.
So that is what drives the, but that is what drives the sun. Now, after the hydrogen is used up most of it, the sun will fuse helium into a heavier element, and the sun doesn't have enough mass to fuse heavier elements than this. So once the hydrogen and helium fuel is used up, the sun will become a red super giant and eventually the outer layers will fly off into outer space and what will be left behind will be a white dwarf and that will be the end of the sun's Existence as a star, that's how it will slowly cool down now, when you have a star that is between 10 and 25 solar masses, it is able to fuse heavier and heavier elements, so it keeps it goes on fusing heavier elements to uh, create energy, fusion energy. Until it reaches the element of iron and iron, basically uh to fuse iron, it takes more energy than the fusion reaction is able to give out. So iron is basically nuclear ash and once a star starts creating iron in its core.
Its lifetime can be measured in milliseconds, so once the iron is formed in the core of a star, which is between 10 and 25 solar masses, it within a fraction of a second, its energy output seizes and this entirety of the star. All the outer layers. Enormous outer layers that are being pushed out and held up by this by the energy of the fusion reaction. They all collapse onto the core of the star and they collapse onto the core of the star and then they bounce out. And that is a supernova explosion. And what's left behind at the core is a neutron star, so this is called a type 2 supernovae. If a star is heavier than 25 solar masses, you won't have a neutron star which will form at the center.
It will be a black hole. Now, if you have a star now, what is a type 1 supernova, a type 1 supernova is a strange supernova in which you have a large star and a neutron star that uh and a white dwarf and a white dwarf that are orbiting each other. So it's a binary star system, two stars, a regular star and a white dwarf. So let me show you what this looks like hang on. Let me make this yeah here we are so you have a regular star here. If you can see the image - and it is, has a companion star, which is a white dwarf, a small one, and in this system the white dwarf star is stealing material from its companion star, okay. So this is the that type of this is that that type of system - a binary system, two stars in which the white dwarf is stealing material slowly from its companion star.
Now there is something called the Chandrasekhar limit, which is 1.4 solar masses, which is as big as a white dwarf can get. Now. This white dwarf is stealing material from its companion star, so it's getting larger once it reaches the Chandrasekhar limit and exceeds the limit. It essentially vaporizes in an enormous explosion, and that is called a type 1 or type 1a supernova. It'S also called a standard candle because we know exactly how much luminosity it will have.
So this is a type 1 supernova, a white dwarf detonates and destroys its companion star in the process. That'S a type 1 supernova. Now we have a third type of supernova, which has been hypothesized, but it seems to have been discovered recently. So this is a star which is between 8 and 10 solar masses. Now a star is basically when it is so. It is basically held up by electron degeneracy pressure, which is a quantum effect in which electrons don't want to be too close together. So they push against uh the star's exterior and that's what holds the star into this in this shape.
Now, when certain uh nuclear reactions happen, so basically I'll tell you about quantum degeneracy, what it is all the matter that we see it is able to have a certain shape because of quantum degeneracy pressure. So that is a quantum effect which gives the universe and the world that we see the shape. It is its. What makes matter solid. It is not electrostatic repulsion. It is quantum degeneracy pressure that that gives solidity to matter.
So it is a quantum effect that we actually see in real life, even though we don't realize it. So this electron degeneracy pressure basically pushes back against the outer layers of the star which want to fall back inside, but in this type of star between 8 and 10 solar masses at a certain stage. What you have is that you have electron capture a nuclear reaction that starts happening in which certain heavy elements start capturing electrons and these electrons fuse with protons and produce neutrons. So suddenly this electron degeneracy pressure, which is holding the star up it vanishes and the star implodes and then explodes so there is a third type of supernova that has recently most likely been discovered. It'S called an electron capture supernova, so it seems that we have finally detected this type of supernova. We even I'm not sure what is left behind at the end of this thing is a white dwarf. Left behind is something else left behind.
I think it's still a matter of conjecture, but this is what it is: the type 3 supernova and electron capture supernovae