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Stellar Evolution

A typical star exists for billions of years, astronomers will never be able to observe one star throughout it's entire life time. Instead they have developed theories about the evolution of stars by studying the stars in different stages of development.

Cason Doyle

on 21 April 2010

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Transcript of Stellar Evolution

Classifying Stars Star Formation Leminosity-the total amout
of energy a star gives
off each second.
Main sequence - the location
on the H-R diagram where
most stars lie.Astonomers use the H-R
diagram to describe the
life cycles of stars. A star begins in a nebula,
a cloud of gas and dust.
When an outside force,
such as the explosion of a
nearby star compresses the
cloud, some of the particles
move close to each other and
are pulled together by gravity.
The shrinking, spinning region
begins to flatten into a disk
that has a central concentration
of matter called a photostar. The Main-Sequence Stage The second and longest stage in the life of a star is the main-sequence stage. During this stage, engery continues to be generated in the core of the star as hydrogen fuses into helium. The stages in the life of a star cover an enormous period of time. Leaving the Main Sequence A star enters the third stage
when almost all of the hyrdogen
atoms within its core havefused into helium atoms.
Giant-a very large and bright star whose hot core has used
most of its hydrogen. Giant stars are above the main sequence
on the H-R diagram. Main-sequence stars that are more massive than the sun will become larger than giants in
their third stage. These highly luminous stars
are called supergiants.
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