ASTRON 1101 Lecture Notes - Lecture 26: Stellar Evolution, Star Cluster, Carbon-Burning Process
29 Oct 2016
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Its luminosity and temperature on the main sequence. Whether it becomes a giant or a supergiant. If it will become a core collapse supernova. What remnants it leaves behind tnuc = 10 gyr (m/msun)-3. Live for a few million years, end as neutron stars or black holes. Live for ten billion years, end as white dwarfs. Live for trillions of years, will end (eventually) as white dwarfs. M > 8 msun (fusion all the way to iron and nickel) One challenge in testing our models is the long times involved. One way to test models of stellar evolution: look at h-r diagrams for star clusters. Star cluster = a group of stars that formed at the same time in the same molecular cloud. Star clusters tell us how stars of different mass look at the same age (plus chemical composition) Open clusters contain hundreds or thousands of stars, and are 10 light years across.
