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Life Cycles of Stars The Hertzsprung-Russell Diagram How Stars Form • Collapsing gas and dust cloud • Protostar mostly infrared Main Sequence Stars • Brown Dwarf • Red Dwarf • Normal Star All Objects Exist Because of a Balance Between Gravity and Some Other Force • • • • • People, Planets-Interatomic Forces Normal Stars-Radiation White Dwarfs-Electron Repulsion Neutron Stars-Nuclear Forces Black Holes-No Known Force How Stars Die • Main Sequence Stars Brighten With Age • The More Massive a Star, the Faster it Uses Fuel • Giant Phase • White Dwarf • Supernova – Neutron Star - Pulsar – Black Hole Historical Supernovae • • • • • 1006 - Chinese 1054 - Chinese, European, Anasazi? 1572 - Tycho’s Star 1604 - Kepler’s Star 1987 - Small Magellanic Cloud (170,000 l.y.) Life (Briefly!) Near a Supernova • Sun’s Energy Output = 77 billion megatons/second • Let’s relate that to human scales. What would that be at one kilometer distance? • 77 x 1015 tons/(150 x 106km)2 = 3 tons • Picture a truckload of explosives a km away giving off a one-second burst of heat and light to rival the Sun Now Assume the Sun Goes Supernova • Brightens by 100 billion times • Our 3 tons of explosive becomes 300,000 megatons • Equivalent to entire Earth’s nuclear arsenal going off one km away - every second • This energy output would last for days Planetary Systems • • • • • Protoplanetary Disks Accretion of Planets Expulsion and Migration of Planets About 30 extrasolar planets known Our Solar System may be unusual? Protoplanetary Disks in Orion