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Gliese 710
3
Transcript
Spectral Class
K5
Work Cited
http://www.solstation.com/stars2/gl710.htm
Life of a Small Star
http://astronomy.swin.edu.au/cosmos/s/solar+mass
Luminosity Class
http://www.astro.keele.ac.uk/workx/starlife/StarpageS_26M.html
Mass
1.Star is born in a region of high density Nebula
Gl 710 has 0.4 solar masses and the Sun has 1
(Normal 0.084)
0.042 compared to sun
2. A region of condensing matter will begin to heat up and start to glow forming Protostars
Gliese 710
3. nuclear reactions occur and hydrogen fuses to form helium.
Temperature
4.The star begins to release energy, stopping it from contracting even more and causes it to shine. It is now a Main Sequence Star.
Age
4,250 K
5.A star of one solar mass remains in main sequence for about 10 billion years, until all of the hydrogen has fused to form helium.
Gliese 710 is relatively a dim star, and a main sequence orange-red or red dwarf star.
6.The helium core now starts to contract further and reactions begin to occur in a shell around the core.
7.The core is hot enough for the helium to fuse to form carbon. The outer layers begin to expand, cool and shine less brightly.
The star was first designated as BD-01 3474 in a catalog that was originally published in 1863 by Friedrich Wilhelm August Argelander.
8.The helium core runs out, and the outer layers drift of away from the core as a gaseous shell
9.The remaining core is now in its final stages. The core becomes a White Dwarf the star eventually cools and dims. When it stops shining, the now dead star is called a Black Dwarf.
Gliese 710
By: Emanuel Cliette
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