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Stellar Evolution Structure Mass governs a star’s temperature, luminosity, and diameter Hydrostatic Equilibrium – the balance between gravity squeezing inward and pressure from nuclear fusion and radiation pushing outward Hydrostatic Equilibrium Star Formation Nebula – a cloud of interstellar gas and dust where the formation of a star begins, when it collapses on itself due to its own gravity Nebula Protostar a rotating disk shape with a hot condensed object at the center formed when the nebula cloud contracts The condensed object becomes a new star Fusion begins when the temperature inside the star becomes hot enough Protostar Star Our Sun’s Lifecycle (part 1) Nebula Protostar Main sequence star – Fusing Hydrogen into Helium Expands into a Red Giant Outer layers are driven off Star contracts back to normal size – Fusing Helium into Carbon Our Sun’s Lifecycle (part 2) A Sun size star will never be hot enough to fuse carbon Outer layers are driven off forming a Planetary Nebula Forms a White Dwarf about the size of Earth – No longer nuclear – Supported by resistance of electron being squeezed together Becomes a Black Dwarf when it runs out of energy Red Giant Planetary Nebula White Dwarf Supergiant Massive Star Lifecycles Several Red Giant phases When the core of a massive star has formed iron, no more reactions can occur, and the core violently collapses in on itself Supernova – a massive explosion that blows off the outer portion around a neutron star Supernova Neutron Star Forms quickly when the collapse of a supernovae is halted due to the neutrons being tightly squeezed together – Extremely dense – 100 trillion times more dense than water – Very small – a radius of approx. only 10km Neutron Star Black Holes Black Holes are formed by the most massive stars (20 times the size if the Sun) The collapse of the star continues forever with gravity that is so immense the not even light can escape it Black Hole http://www.youtube.com/watch?v=f_KLOFe2rDY