Fusion: Creating a Star on Earth - General Atomics Fusion Education

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Energy Release E = mc 2 0.008 Hydrogen 0.006 Deuterium Extra mass per nucleon 0.004 0.002 0 Tritium Lithium Uranium - 0.002 0 40 80 120 160 200 240 Atomic mass number 36
<strong>Fusion</strong> Energy Input We give kinetic energy (temperature) to hydrogen Energy Output We get back 2000 times more energy than we put in 37
Page 2: Fusion: Cr
Page 9 and 10: Alternative Energy Sources • Hydr
Page 11 and 12: Energy Source Advantages and Disadv
Page 13 and 14: Fusion Energy The
Page 17 and 18: In a typical fission process used a
Page 19 and 20: Fusion Atom + ENER
Page 21 and 22: Comparison of Long-Term Energy Sour
Page 23 and 24: e 2 orbitals with 2 electrons each
Page 25 and 26: Plasma Makes up The Sun & S
Page 28: Like Charges Repel 28
Page 31 and 32: Hydrogen = 1H 1 Deuterium = 1H 2 Tr
Page 33 and 34: Summary of Solar Fusion</st
Page 35: E = mc 2 Einstein’s equation that
Page 39 and 40: Abundant Energy From Sea Water 50 C
Page 41 and 42: Heat Exchanger Neutron Heat Exchang
Page 43 and 44: Deuteron Energetic Neutron
Page 45 and 46: Methods to Heat Deuterium-Tritium F
Page 47 and 48: High Power Lasers can Deliver the I
Page 49 and 50: Inertial Confinement Fusion
Page 51 and 52: Typical Plasmas Density n e (m -3 )
Page 53: Unconfined Confined Ion Electrons M
Page 56 and 57: List of Major Programs/Devices Worl
Page 58 and 59: TFTR is located at PPPL Princeton,
Page 60 and 61: ITER (International Thermonuclear E
Page 62 and 63: ITER 63
Page 64 and 65: What Progress Has Been Made in Magn

Fusion: Creating a Star on Earth - General Atomics Fusion Education

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