Schönberg–Chandrasekhar limit
When stars are born, they are made up of gas and dust that come together due to gravity. This gas and dust start to get really hot and create energy from the center of the star. This energy pushes out and stops the star from collapsing in on itself.
As the star gets older, it starts to run out of the gas and dust that it needs to make energy. Eventually, when a star runs out of gas and dust, it starts to shrink inward, slowly and peacefully.
However, some stars are bigger than others, and the more massive the star, the more it will shrink inward. This shrinking process creates a lot of heat, and if the star is big enough, the heat can be so intense that it creates nuclear reactions, which means atoms are being smashed together to make new ones.
This nuclear reaction produces an enormous amount of energy which completely stops the star from collapsing inward. But at some point, the star can't create any more energy from fusion, and it starts to collapse in on itself again.
If a star is massive enough, this collapsing inward process can generate even more heat, which leads to even more nuclear fusion. But eventually, the star will run out of fuel, and no amount of heat and pressure can make new energy.
This is where the Schönberg–Chandrasekhar limit comes in. This limit is the point where a star is so massive that it can't generate enough heat and pressure to stop itself from collapsing in on itself completely.
When that happens, the star collapses, and all of the material in it is compressed into a very small space. This creates an incredibly dense object called a neutron star or a black hole.
So, to sum it up, the Schönberg–Chandrasekhar limit is the point where a star is so massive that it can't generate enough heat and pressure to stop itself from collapsing, which leads to the creation of a neutron star or a black hole.
As the star gets older, it starts to run out of the gas and dust that it needs to make energy. Eventually, when a star runs out of gas and dust, it starts to shrink inward, slowly and peacefully.
However, some stars are bigger than others, and the more massive the star, the more it will shrink inward. This shrinking process creates a lot of heat, and if the star is big enough, the heat can be so intense that it creates nuclear reactions, which means atoms are being smashed together to make new ones.
This nuclear reaction produces an enormous amount of energy which completely stops the star from collapsing inward. But at some point, the star can't create any more energy from fusion, and it starts to collapse in on itself again.
If a star is massive enough, this collapsing inward process can generate even more heat, which leads to even more nuclear fusion. But eventually, the star will run out of fuel, and no amount of heat and pressure can make new energy.
This is where the Schönberg–Chandrasekhar limit comes in. This limit is the point where a star is so massive that it can't generate enough heat and pressure to stop itself from collapsing in on itself completely.
When that happens, the star collapses, and all of the material in it is compressed into a very small space. This creates an incredibly dense object called a neutron star or a black hole.
So, to sum it up, the Schönberg–Chandrasekhar limit is the point where a star is so massive that it can't generate enough heat and pressure to stop itself from collapsing, which leads to the creation of a neutron star or a black hole.