lecture08 - Sun Power I Stars Light Sun light spectrum...

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ENGRI 1290 1 Sun Power I Stars Light Sun light spectrum
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ENGRI 1290 2 Lecture’s objectives • Learning the physical mechanisms that power the stars • Understanding what are electromagnetic radiations • Discovering which part of the Sun’s light spectrum can be used to produce energy
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ENGRI 1290 3 Stars in the universe • The observable universe is quite large – 92 billion light years • The many “engines” of the universe –Da rk Ene rgy ?? – Black holes –S ta
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ENGRI 1290 4 Fusion in the sun (proton cycle) ν ν γ γ The hydrogen in the sun is hot ~ 14MK. It is not in the state of a gas but rather fully ionized (plasma). The electrons and the protons cannot bound due to the large number of proton-electron collisions. These collisions are so energetic that two protons can fuse to give 2 H (deuterium). A positron and a
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This note was uploaded on 09/14/2011 for the course ENGRI 1290 taught by Professor Gourdain during the Fall '10 term at Cornell University (Engineering School).

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lecture08 - Sun Power I Stars Light Sun light spectrum...

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