Red Dwarf Stars - KevinHutchinson Why have no main sequence stars of spectral class M have yet evolved into red-giants stars We know that stars of the

Red Dwarf Stars - KevinHutchinson Why have no main sequence...

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Kevin Hutchinson 3/29/14 Why have no main sequence stars of spectral class M have yet evolved into red-giants stars? We know that stars of the spectral class M have the longest lifetimes of all stars but why makes them so special and different from other main-sequence stars? What can their long lifetimes call us about our universe? First I get an understanding of the make up and qualities of a class M star and compare that to other stars particularly red supergiant. Then I must dig deeper to find what the information about the lifetime and lives of these spectral class M stars can tell us about our own planet. The very first stars in our universe derived molecular clouds composed of hydrogen and helium in space. Those first stars then use that hydrogen and helium to create other elements that would later on be components of the future stars of our universe. Stars form when gravity causes a molecular cloud to contract until the center of the contraction becomes hot enough to sustain energy in its core. This core is made out of helium and hydrogen. Unfortunately for most stars, the same gravity that once helped them become formed can also lead to their destruction and also the end of their lifetime. The force of gravity forces all of this nuclear fusion in the core of the star to be compressed creating more energy but if this energy doesn’t get released, the star collapses within itself. Stars must use capture this thermal heat and prevent it from being radiated from outside of the cloud. By making its core dense enough to trap almost all of the radiation inside it, the pressure and temperature of the star will increase and will push back against the forces of gravity, slowing the contraction. This new energy formed is now a protostar and eventually will become a star when it becomes hot enough. Let me start off by describing the process of formation of low mass stars. Most stars in the main sequence stars, which are tars that are fusing hydrogen atoms to form helium atoms in their cores. Most of the stars in the universe about main sequence stars. During the 20
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  • Fall '09
  • Astronomy, online service, Springer New York

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