The Lives of Stars
The Lives of Stars Astr 1010-100
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This 2 page Class Notes was uploaded by Alyssa Karounos on Friday February 13, 2015. The Class Notes belongs to Astr 1010-100 at University of Washington taught by Dr. Oliver Fraser in Winter2015. Since its upload, it has received 138 views. For similar materials see Introductory Astronomy 1 in Astronomy at University of Washington.
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Date Created: 02/13/15
21115 1 Goals A B Identify the major steps of stellar evolution in name and on the HR diagram Rank the ages of clusters based on their colormagnitude diagram 11 Electrons only change their levels When they interact with light of the correct wavelength because it proves the right amount of energy to change levels 111 Star Clusters A The ColorMagnitude diagram of clusters are useful because all the stars have the same distance 1 We actually measure their relative luminosity Main Sequence TumOff 1 at the top of main sequence Where stars don t adhere to the Main Sequence line 2 difference in angle of turn off per cluster C Masses of stars in main sequence typical pattern F T Erma K L ALuminosily m AM ass 100 0 stars put out a million times more energy per mass than M stars 1 losing more energy faster stars are all burning their fuel and run out so they move to the right of the Main Sequence peeling off and turn into giants giants move evolved than those underneath In a cluster Main sequence stars are all the same age clusters are form from molecular clouds at the same time but the big ones evolve first temperature of atmosphere is determined by the mass 1 mass determines temperature Which determines differences the deeper in you go the more atmosphere this is and the more pressure there is M stars create nuclear fusion all the time IV What happens When a star runs out of Hydrogen in its core A normally burning produces pressure that balances weight 1 hydrodynamic equilibrium burning turns off pressure goes down star settles around the core cores is made of helium because of the He ash that the hydrogen burned 959 the core is going to get hot enough to burn again but this time with a shell of hydrogen around the helium core star burning faster with more luminosity 10 of mass is under the layer of it expands and become giants once you burn out all hydrogen cores and move to helium core you go off the main sequence B What happens when a star runs out of Hydrogen in the shell 1 pWNQP y xy x HO r tr t UJN j A J helium core got so big that hydrogen cooled off makes things tight now it will burn helium and back to equilibrium very quick change small transition all sunlike stars that we know will do this helium core buming using energy much faster runs out of helium core burn what is carries becomes tight Not hot enough to keep burning heads back to right and has two shells core of carbon that does nothing and Helium ring around Carbon a two shells every time you burn in a shell Giant star double shell puffs out atmosphere and molecules a planetary nebula loss of atmosphere and are left with core a becomes white dwarf
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