Stellar Evolution

The beginning of the star's evolutionary star is a very slight interstellar gas and dust particle distribution during a dozen light years. There is a very low pressure between the stars, but this gas distribution is not a true vacuum. When the gas density exceeds 0.1 particles per cubic centimeter, the interstellar gas becomes unstable. There is also a small deviation in density, and since it is not possible to have a completely uniform distribution in these clouds, this will occur naturally and the region will begin to shrink.

Observing stars by calculating star models makes it possible for astronomers to understand the evolution of stars. Star evolution is the process by which pressure (gravity) changes stars. As these forces acted on the stars their properties changed dramatically during their existence. The evolution of stars in the form of these fuel consumption phases and their finalization is very important. Because it is responsible for producing most elements (all elements after H and He). In addition, the various stages of a star's life cycle are an important part of the formation of galaxies, new stars, and planetary systems.

Star evolution as a species has never actually witnessed the whole process of evolution of stars. This is because stars may survive millions of years from birth to death. Still, Lutgen and Tarbuck (2011) pointed out that we were able to design the stellar evolutionary stage based on the various stages we can observe the stars. It is speculated that these stages are intended to produce the evolutionary processes of stars. Stage: A star is born

Evolution of stars has not been studied by observing the life span of a single star because most stellar changes are too late to discover for centuries. Instead, astrophysicists use a computer model to simulate the structure of stars and understand how stars evolved at various points in the life cycle. The evolution of a star begins with the collapse of the gravitational force of macromolecular clouds. A typical macromolecular cloud is about 100 light years (9.5 x 1014 km) and contains up to 6,000,000 solar masses (1.2 x 1037 kg). When it collapses, huge molecular clouds divide into smaller fragments. In each of these fragments, the collapsed gas emits gravitational potential energy as heat. As the temperature and pressure rise, the debris condenses into a rotating sphere called the star of the primitive star.