AST101H1 Lecture Notes - Lecture 10: Nuclear Fusion, Thermostat, Differential Rotation

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AST101H1 Full Course Notes
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AST101H1 Full Course Notes
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Nuclear fusion keeps the sun"s core at about 15 million k. Fusion: sticking nuclear particles together: particles have to be moving super fast to fuse; temperature is really a measure of. October 10, 2013. how quickly particles are moving. How hot is the sun: 6000 k, 10 000 k, 1 000 000 k, or 15 000 000 k, all of the above depending on core, outer layer, etc. If the sun"s core got a little hotter, what would happen: the fusion rate would increase until the core expanded, then it would slow down. We can see the sun because it emits light: whereas the moon reflects light, a window pane transmits light, as in light passes through it. Huuuuuge orbs that are tanks of water lined with basically cameras that look out for. Every week or two particles collide and give off the tiniest bit of light and all the cameras take pictures.

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