What is the star evolution?
Stellar Evolution describes the process in which the stars are formed, burn for a long time and eventually die. Along the way, the star is struggling with the certificate of gravity and fuel in an effort to maintain balance. A lot of stellar evolution is theory, because people were not long enough to observe the entire life cycle of a single star, but thanks to a large number of stars in different stages scattered around the universe it was possible to make educated estimates about how the stars develop over time, and the process is relatively predictable. The stars are formed in the so -called "giant molecular clouds", swirling mass of gases and particles. Over time, these clouds are subject to gravitational collapse, creating protostars, heavenly bodies that have the potential to become stars. The type of star in which the Protostar develops depends on its chemical composition. When the star gradually stretches, a number of nuclear reactions begin to occur, causing the star to gain luminosity.
NakOneC will consume its fuel, usually collapse and release another chain reaction of events that cause the star to burn extremely hot and bright. Depending on the type of star, it can turn into a white dwarf, a neutron star or a black hole when it dies, often preceding this event with a fantastic supernum caused by a chain reaction escape. Starry development is constantly found all over the universe when the stars come and leave.
Every phase of a star life can be brought into a graph like Hertzsprung-Russel diagram. The graph compares color, size, luminance and star temperature. The stars of a certain class tend to combine on such diagrams and demonstrate clear relationships between specific types of stars that can be used to Lemurn more about stars in general. Using such a graph, scientists can take observations of different stars and convert them over a distance from the ground and other useful star development data.
Many stars fall into the classification known as the main sequenceE with reference to a signature cluster of stars that can be seen on many charts used to map stars according to the characteristics. The sun is an example of the main sequential star and, according to most estimates, remains stable for at least five billion years. At the end of the main sequential period, the sun is converted into a red giant and expands significantly because it uses its fuel and absorbs several planets, including Earth, along the way.