Life of a Star

The most common star is our own sun, which is common sense, but where does the sun come from? It can not come out of thin air, it can not exist forever, as all birth leads to death. Astronomers believe that molecular clouds or massive natural gas clouds are the main cause of the birth of stars. Gravity compresses this cloud into giant gas and dust spheres; when the temperature reaches 15 million degrees it causes nuclear fusion, which starts to burn with glow.

The life cycle of a star depends on its quality. The higher the quality, the shorter the life cycle. The quality of stars depends on the mass of the material available in the nebula, the huge gas it produces and the dust cloud. Eventually hydrogen in the nebula will be drawn together by gravity and start to rotate. As the gas rotates faster, the gas is heated to become the original star. The final temperature reaches 15,000,000 degrees and nuclear fusion occurs in the center of the cloud. Clouds start to shine, shrink a little, and stabilize. It is a major binary star at present and is shining for millions to billions of years at this stage. This is the stage where our sun is now.

Scientists say that stars will be resurrected when gas clouds collapse to form the original stars. As the primitive star continues to crash, it enters the "main line" stage. This is where the stars illuminate most of the night. Main line stars have a long life under human standards but these stars will go through several cycles before they finish their lives. Hydrogen bombs and main line stars have one thing in common. They are to generate enormous amounts of energy by fusing hydrogen atoms. The sun like Sirius is the main star. The higher the quality of the main line star, the more it looks blue. For example, Sirius is bigger than the sun, but it is more blue than the sun. These types of stars have limited supply of hydrogen to supply fuel to the fusion process. When hydrogen runs out, the color of the main line star changes to red, making it a brighter superstar.