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Chapters 14 and 15 Stellar Evolution and Stellar Remnants

Chapters 14 and 15 Stellar Evolution and Stellar Remnants. Star Birth: Nebula. Young star: Protostar. Adult: Main Sequence .

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Chapters 14 and 15 Stellar Evolution and Stellar Remnants

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  1. Chapters 14 and 15 Stellar Evolution and Stellar Remnants

  2. Star Birth: Nebula

  3. Young star: Protostar

  4. Adult: Main Sequence • As the temperature in the interior rises, nuclear reactions produce outward force and balances the inward force of gravity  hydrostatic equilibrium = star becomes stable and contraction stopsmain-sequence star

  5. Energy Sources in Stars • 4 hydrogen nuclei fuse to become 1 helium nucleus • Since the mass of 4 hydrogen nuclei is greater than the mass of 1 helium nucleus, the leftover mass (0.7%) is converted to energy by Einstein’s equation: E=mc2

  6. The end states of stars depends upon its mass! The more massive a star, the faster it consumes its fuel, the shorter its lifetime

  7. A B C

  8. Evolution of Low Mass Stars including our Sun M < 10 Solar Masses

  9. Old Age: Red Giant

  10. Elderly, core: White Dwarf The core of the white dwarf star is now all carbon and oxygen

  11. Elderly, envelope: Planetary nebula Ring Nebula Eskimo Nebula

  12. Yeah, but what about the really Massive stars?

  13. Old Age: Red Supergiant

  14. Figure 13.19 Elderly, dying star:Supernova

  15. Super Nova Remnants

  16. Our Sun will never explode. Only massive stars explode as supernova!

  17. Elderly, core: Neutron Star Core High mass stars becomes so dense that protons and electrons combine to become neutrons and star becomes neutron star

  18. Life Cycle of a Low Mass Star

  19. Life Cycle of a High Mass Star

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