What is carbon burning?
The carbon combustion process is a nuclear reaction that occurs at the core of massive stars under huge temperature and pressure conditions. The combustion of carbon initiates only at the end of the life of the star. In order for the star to build sufficient pressure in its core to start the carbon burning, it must contain at least four solar materials at birth. The carbon burning only starts after the burning of large parts of hydrogen and helium star.
The most abundant element in the universe is hydrogen. So most stars begin their lives consisting mainly of hydrogen. When the nuclear fusion ignites in the core of a young star, hydrogen slowly starts to burn, its atomic cores connect into helium through the P-P-P-in the stars the Sun Weight or the less-or CNO cycle-in the massive stars. This is a nuclear reaction that generates solar heat and light we see when we get out every day.
Depending on the size of the star, it burns nuclear fuel at a different speed. Massive stars have thicker and warmer centers and burn their fuel Rybread. Some of the biggest stars exhaust most of their hydrogen fuel within a few million years, while the sun is to continue joining hydrogen for 4.5 billion years and the lightest stars combine hydrogen for a trillion years. When Helium accumulates "ashes", it eventually reaches critical density to cause the helium ignition. Helia burn products are carbon and oxygen.
When carbon and oxygen are accumulated in the core of the star for millions of years of combustion of helium, a large percentage of helium is exhausted and the stars core cool down and cannot generate more nuclear energy. This cooling causes the nucleus to download, which further increases density and pressure. In the stars above about four sunshs, tap temperatures and density is achieved for carbon burning. This warms the core of the star and expands and becomes a red supergiant.
Carbon combustion is one of the main reasons why there are elements heavier than carbon in space. The main reaction consists of several components.In one, two carbon cores of the fuse are formed atom neon and atom Helia. Finally, these fall into sodium and hydrogen, then magnesium and free neutron. Due to all nuclear processes, it takes place at the same time in the core of the star, produced large amounts of neon, oxygen and magnesium. The entire carbon combustion process takes only about 1000 years.
If a star has a material between four and eight solar masses, it excludes its outer layer when Peters burn carbon, create a planetary nebula and leave behind a white dwarf core. If it has more than eight solar materials, it will eventually start neon burning, another phase of the development of massive Stars.