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Astronomy 3.4 Evolution of Stars

astronomy-3-4-evolution-of-stars

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How Stars are formed...

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Star reaches stable size
Temperature at core reaches 15 million k. Fusion starts
Gas cloud begins to collapse and breaks up into protostars
Outward pressure from radiation prevents any further collapse - Main sequence star is formed
Rise in temperature and pressure as GPE (gravitational potential Energy) KE (kinetic energy)
Stars are formed from huge clouds of gas and dust called nebulae - Found mainly in spiral arms of Galaxy e.g. Orion’s nebula

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Describe a stars death...

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Temperatures at core rise to 100 million kelvin - Helium nuclei fuse to form carbon.
Fusion restarts in a shell surrounding the core which is now rich in helium.
Helium is depleted - Red giant loses it’s outer layers in an expanding shell of gas - Planetary nebula
Core collapses to form White Dwarf - Cools eventually to brown and then black.
No radiation countering gravitational collapse
Temperature rises further
Star runs out of Hydrogen
Outer layers of the star expand and cool to form red giant.
FINAL Mass of star affects how star dies Super giants can form iron through fusion Supernova! Then Neutron star or Black Hole.
Star collapses

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What is a supernova?

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What is a Neutron star?

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How can we deduce the chemical composition of a star?

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How can we deduce the temperature of a star?

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How can we determine the radial velocity of a star?

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Describe the Harvard classification of Spectral type.

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What is a HR diagram?

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Draw a HR / Hertzsprung–Russell diagram

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Which stars will run out of fuel sooner?

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Give evidence for the existence of Neutron stars.

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Give 3 pieces of evidence for the existence of black holes

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