Notes from study session: earth history Big bang nucleosynthesis: Life of a star: formation after H fusion; will stay in that phase for most of its lifetime. (converting H to He); rate at which we are doing that today is much smaller than happened in the first 3 minutes; we can take the He (3) stick them together and get a more massive nuclei = 12 Carbon make more massive things by fusing them together. You can get as far as Si and then get to Fe (Iron) because it is the most stable form of energy. Volatile : how quickly something evaporates Pleides is a constellation. (a group of starts (hot young passing through gas cloud)) Matter era begins about 3 or 4 minutes 380,000 is the time at which H atoms really form. After this, the photons don’t interact with matter.
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This note was uploaded on 02/27/2008 for the course GEOL 125Lxg taught by Professor Hammond during the Fall '07 term at USC.