Stellar evolution: Difference between revisions
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Stellar evolution can be described as the birth, life, and death of a star. A period that can last from ten billion to a few hundred billion years depending on its size. Our Sun is about 4.5 billions years old and should last us another six billion years, making our Sun an average star amounst the bounty and variety of stallar mass in our galaxy, the Milkyway. | |||
Throughout a star's life, the star fearsly consumes it hyrdrogen through the process of neclear fusion in its core, creating new and heavier elements until the star has exhausted all its fuel. The end of a star's life again depends on the star's size, for example; our sun will most likely become a red giant and then slowly shrine for another few millions year and become a dark cinder called a brown dwarf. Yet other stars with much larger masses of about ten times that of our Sun's have an increased chance that it may burst and eject all its stallar material into surrounding space leaving behind a super dense object called a neutron star. | Throughout a star's life, the star fearsly consumes it hyrdrogen through the process of neclear fusion in its core, creating new and heavier elements until the star has exhausted all its fuel. The end of a star's life again depends on the star's size, for example; our sun will most likely become a red giant and then slowly shrine for another few millions year and become a dark cinder called a brown dwarf. Yet other stars with much larger masses of about ten times that of our Sun's have an increased chance that it may burst and eject all its stallar material into surrounding space leaving behind a super dense object called a neutron star. | ||
Revision as of 06:21, 14 May 2007
Stellar evolution can be described as the birth, life, and death of a star. A period that can last from ten billion to a few hundred billion years depending on its size. Our Sun is about 4.5 billions years old and should last us another six billion years, making our Sun an average star amounst the bounty and variety of stallar mass in our galaxy, the Milkyway. Throughout a star's life, the star fearsly consumes it hyrdrogen through the process of neclear fusion in its core, creating new and heavier elements until the star has exhausted all its fuel. The end of a star's life again depends on the star's size, for example; our sun will most likely become a red giant and then slowly shrine for another few millions year and become a dark cinder called a brown dwarf. Yet other stars with much larger masses of about ten times that of our Sun's have an increased chance that it may burst and eject all its stallar material into surrounding space leaving behind a super dense object called a neutron star.