Stellar Fusion
Process and importance of fusion in stellar evolution.
Huge clouds of hydrogen atoms and gravity cause the atoms to be attracted to each other creating them to slowly move towards the centre of mass.The atoms then continue condensing until something happens.All of the atoms are trying to get to the centre of mass. While this is happening the temperature becomes 10 million Kelvin and at that point there is enough temperature and enough pressure to overcome the coulomb forces, bringing the two protons close enough to each other for the fusion process (diagram below). This is called ignition because when two of the protons fuse the resulting nucleus has a slightly smaller mass. So the first stage of this there are two protons under enough pressure …show more content…
Everyday more and more is being discovered about stellar evolution expanding the stellar knowledge for all scientists. One of the main reasons a star collapses is because it has run out of fuel in the core, this then collapses because the fusion acts as a support force against gravity, also anything with mass will have a gravitational force then once the fusing process stops gravity is able to begin to compress the star. While this is happening the conservation of angular momentum takes place and the rate of spin then increases. Conservation of angular momentum is when a star is spinning on and angle and over time, it slowly gains speed, While its angular momentum continues to stay the same, this usually leads to black holes. Angular momentum is the rotation around a point. On rare occasions the supernovae explode and pulsars are formed from that explosion. As the pulsars decrease in size they begin to spin faster because of the conservation of angular momentum. Astronomers use spectroscopy to help aid with distant stars and galaxies. It is used by the different wavelengths and the study of visible light and shows us many things such as temperature, chemical composition, mass, distance and much more. This is also current knowledge of physics theories of the different stages of stellar
Huge clouds of hydrogen atoms and gravity cause the atoms to be attracted to each other creating them to slowly move towards the centre of mass.The atoms then continue condensing until something happens.All of the atoms are trying to get to the centre of mass. While this is happening the temperature becomes 10 million Kelvin and at that point there is enough temperature and enough pressure to overcome the coulomb forces, bringing the two protons close enough to each other for the fusion process (diagram below). This is called ignition because when two of the protons fuse the resulting nucleus has a slightly smaller mass. So the first stage of this there are two protons under enough pressure …show more content…
Everyday more and more is being discovered about stellar evolution expanding the stellar knowledge for all scientists. One of the main reasons a star collapses is because it has run out of fuel in the core, this then collapses because the fusion acts as a support force against gravity, also anything with mass will have a gravitational force then once the fusing process stops gravity is able to begin to compress the star. While this is happening the conservation of angular momentum takes place and the rate of spin then increases. Conservation of angular momentum is when a star is spinning on and angle and over time, it slowly gains speed, While its angular momentum continues to stay the same, this usually leads to black holes. Angular momentum is the rotation around a point. On rare occasions the supernovae explode and pulsars are formed from that explosion. As the pulsars decrease in size they begin to spin faster because of the conservation of angular momentum. Astronomers use spectroscopy to help aid with distant stars and galaxies. It is used by the different wavelengths and the study of visible light and shows us many things such as temperature, chemical composition, mass, distance and much more. This is also current knowledge of physics theories of the different stages of stellar