Chapters 14 and 15 Stellar Evolution and Stellar Remnants.

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Presentation transcript:

Chapters 14 and 15 Stellar Evolution and Stellar Remnants

Star Birth: Nebula

Young star: Protostar

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 Adult: Main Sequence

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=mc 2

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

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

Ring NebulaEskimo Nebula Elderly, envelope: Planetary nebula

Yeah, but what about the really Massive stars?

Old Age: Red Supergiant

Figure 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

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