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Transcript
Chapters 14 and 15 Stellar Evolution and Stellar Remnants Star Birth: Nebula Young star: Protostar 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 stopsmain-sequence star 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 The end states of stars depends upon its mass! The more massive a star, the faster it consumes its fuel, the shorter its lifetime A B C Evolution of Low Mass Stars including our Sun M < 10 Solar Masses Old Age: Red Giant Elderly, core: White Dwarf The core of the white dwarf star is now all carbon and oxygen Elderly, envelope: Planetary nebula Ring Nebula Eskimo Nebula Yeah, but what about the really Massive stars? Old Age: Red Supergiant Figure 13.19 Elderly, dying star: Supernova Super Nova Remnants Our Sun will never explode. Only massive stars explode as supernova! Elderly, core: Neutron Star Core High mass stars becomes so dense that protons and electrons combine to become neutrons and star becomes neutron star Life Cycle of a Low Mass Star Life Cycle of a High Mass Star
