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Lecture 10

Lecture 10 - Sun Stuff - October 10.docx

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University of Toronto St. George
Astronomy & Astrophysics
Michael Reid

October 10, 2013. Lecture 10 - The solar spectrum—continuous part Sun  Nuclear fusion keeps the Sun’s core at about 15 million K  Fusion: sticking nuclear particles together o Particles have to be moving super fast to fuse; temperature is really a measure of how quickly particles are moving  Fission: …  How hot is the sun? o 6000 K, 10 000 K, 1 000 000 K, or 15 000 000 K o All of the above depending on core, outer layer, etc.  The solar thermostat stabilizes energy production in the core o A slight drop in core temperature leads to a large decrease in the fusion rate that lowers the core pressure causing the core to contract and heat up thereby restoring the fusion rate to normal  If the Sun’s core got a little hotter, what would happen? o The fusion rate would increase until the core expanded, then it would slow down  We can see the sun because it EMITS light o Whereas the moon REFLECTS light o
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