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Slide 2 1. How do scientists measure our distance from stars that are too far to use the parallax effect? 2. How is this this related to absolute magnitude? Times Up! Slide 3 Slide 4 Make a T-chart On one side list 3 things you think you know about stars. On the other side 3 list things you want to know about stars. Slide 5 Not really empty Stars, planets, etc. Interstellar medium Dust and Gas Nebulas Orion Nebula http://hubblesite.org/gallery/album/nebula/pr19 95044a/ Large Magellanic Cloud http://hubblesite.org/gallery/album/nebula/pr200605 5a/ Slide 6 Nebulae are usually composed of 70% Hydrogen, 28% Helium, 2% heavier elements A force compresses the particles, they begin to contract together Slide 7 Gravity at work More mass means more gravity; more gravity results in more mass, etc. Slide 8 As the Gravitational forces between the particles increase, they begin to spin more rapidly Here is a demodemo The shrinking, spinning region begins to flatten onto a disk called a PROTOSTAR Slide 9 Increased pressure and temperature Temperature continues to increase until it reaches about 10,000,000 O C when NUCLEAR FUSION begins and a star is born! Slide 10 Little mass lots of energy E = mc 2 Slide 11 Fermi National Lab http://www.wired.com/playbook/2012/08/olympics-physics-hammer-throw/ http://www.universetoday.com/52696/nuclear-fusion-power-closer-to-reality-say-two-separate-teams/ High temperatures 2 particles become 1 Releases a lot of energy Slide 12 Energy heats up gas and causes outward expansion. Gravity pushes in. Forces balance out = Hydrostatic Equilibrium Stable adult stage star