1. Life Cycle of the Stars By Aiyana and Meredith http://techcenter.davidson.k12.nc.us/spring026/images/OuterSpace.jpg

2. Nebula A nebula is made of gas and dust The nebula is the birth place of a star They get their light from nearby stars. http://sunshine.chpc.uh.edu/labs/star_life/starlife_main.htmlta http://www.windowsmoviemakers.net/PapaJohn/117/Blue- Screen_Outer_Space_Clips_files/image004.jpg

3. Protostar “Fetus” The protostar is the first stage of a star’s life Formed when gravity clumps the hydrogen and helium of a nebula together In order to grow in life it needs to maintain equilibrium – Balance between gravity pulling atoms towards center and gas pushing heat and light away form center http://sunshine.chpc.utah.edu/labs/star_life/starlife_proto.html

4. Main Sequence “Adulthood” Phase in which stars live out the majority of their lives Stars last in main sequence for billions of years During entire life the star battles gravity, trying to crush it http://spaceflightnow.com/news/n0009/15supernova/supernova.jpg http://www.presentationstation.com/Backgrounds/Miscellaneous_2/orange_spot.jpg

5. Red Giant “Middle Age” During this short phase the star starts cooling and the fusion fuel starts going away Core shrinks but fusion keeps on going When our sun reaches the phase of a red giant its diameter will expand to the size of the orbit of Mars http://sunshine.chpc.utah.edu/labs/star_life/support/red_giant.html http://www.awesomebackgrounds.com/templates/fire-on.JPG

6. White Dwarf/Black Hole “Old Age” When a star runs out of fuel to burn, gravity collapses it in Low mass stars, who have electrons that prevent the collapse of the core, shrink to a white dwarf When crushed by gravity high mass stars totally leave space become a black hole http://spaceflightnow.com/news/n0005/22astronext10/000522blackhole.jpg http://www.vgaplanets.com/v4doc/PLAN0020.gif http://www.freestockfootage.com/Thumbs/t600-100-023.jpg White Dwarf Black Hole

7. Brown Dwarf Star like objects in space that have masses less than.08 times that of the sun Unable to sustain hydrogen fusion Brown dwarf is a protostar that didn’t have enough dust and gas to achieve a temperature hot enough to ignite fusion Arrow is pointing at a Brown Dwarf http://www.universetoday.com/html/pictures/big2002-0109a.jpg

8. Planetary Nebula “After Life” When a star explodes a large cloud of gas is expelled called a Planetary Nebula The first planetary nebula ever seen was the Dumbbell Nebula M27 http://www.ask.com/bar?q=planetry+nebula&page=1&adt=0&qsrc=2417 &ab=0&title=Planetary Nebula&u=http%3A%2F%2Fschmidling.com%2Fplanebs.htm After explosion the core remains extremely hot which emits high energetic radiation One of the largest planetary Nebulae is NGC246

9. Helium fusion Nuclear fusion with the nuclei being involved with helium. Powered by fusing the element hydrogen into the element helium. When stars exhaust their hydrogen fuel and build up a lot of helium, they begin to fuse helium together to form carbon. http://www.oufusion.org.uk/newsspring05/helium2carbon.jpg http://www.awesomebackgrounds.com/ss-explosion.htm

10. Hydrogen Fusion Four hydrogen nuclei come together to make a nucleus. There are electrons, neutrinos, and photons involved in making fusion of hydrogen into helium. This fusion cycle generates energy in our Sun. http://www.physics.uiowa.edu/~umallik/adventure/spangle/spangle_files/image018.gif

11. Neutron Star Neutron stars are objects created in the cores of massive stars. The core of a star collapses and crushes together every proton combined with electrons. Neutrons can stop the collapse and remain as neutron stars.

12. Supernova Most energetic explosion. Occur at the end of a star’s life, when nuclear fuel is exhausted and can no longer be supported by the nuclear energy. When the explosion occurs, the brightness can be as that of many millions of stars. http://www.ask.com/bar?q=supernova+information&page=1&adt=0&qsrc=2417&ab=3&title= Supernovae&u=http%3A%2F%2Fimagine.gsfc.nasa.gov%2Fdocs%2Fscience%2Fknow_l2%2Fsu pernovae.html http://chandra.harvard.edu/photo/2004/rxj1242/rxj1242_still3.jpg