Nuclear Physics, A Very Short Introduction
Frank Close 2015, Tigard Lib 539.7 CLO
- p11 1909-11 Rutherford and Marsden bombard gold foil with alphas, 1/10000 bounce back, demonstrates dense positive nucleus less than 1e-12 by volume.
- p12 1913 Bohr "planetary" model for electron, except solar system planets denser than electrons in atoms
- p13 quarks smaller than 1e-4 nuclear radius
p15 Patrick Blackett 1921-4 23,000 cloud chamber photographs of alphas bombarding nitrogen, eight examples of proton ejection and an oxygen
p19 Chadwick neutron 1932
p23 Pauli hypothesized neutrino 1931
- proton, neutron, electron, neutrino spin 1/2
p25Joliot-Curies irradiated aluminum with alpha (helium) particles from radium (or polonium?), produced phosphorus-30 with 3 minute half life
p26 Al[13p14n] + He[2p2n] => n + P[15p15n] ( 3 min ) => Si[16p14n] + positron + neutrino
- p26 1935 Nobel, Frédéric suggests "transmutations of an explosive type"
p27 Hahn and Strassmann fission 1938, Fermi slow neutrons with paraffin or water so they don't shatter nuclei
027 Lisa Meitner and Otto Frisch liquid drop model, instability, fission
- 028 Planck law E=hv
032 Strong force, neutron stability in nucleus
036 pions emitted when neutrons or protons "pummeled"
037 ΔE × Δt ≈ 140MeV × 1e-23s < h/4π, hence pion range about 1 fm inside nucleus
038 quark binding force increases with distanc
040 Quark-gluon plasma beginning universe
041 Relativistic Heavy Ion Collider gold or lead atoms, 50x density compared to cold nuclei
041 Blue Riband
045 Magic number
- most stable 2 helium, 8 oxygen, 20 calcium, 50 nickel, 82 tin, 126 lead, heavier nuclei unstable
- half lives: Bi209 2e19y, Po209 124y, At219 8h, Rn222 92h, Fr223 22m, Ra226 1600y , Ac227 22y, Th232 14e9y, Pa231 32e3y, U2338 45e8y, Np237 2e6y, Pu239 24e3y, Pu244 8e7y,
- 055 Pairs of opposed spin nucleons have enhanced mutual attraction
- Iron 56 is 26 protons, 30 neutrons
058 Technetium lightest unstable element, τεχνητός =artificial
059 Technetium star (enhanced technetium spectral line)
- 061 Universe first microsecond, equal quantities neutrons and protons, first three minutes surviving neutrons combine with protons
- 062 1e9 neutrinos per formed atom
- 065 at three minutes, 75% protons, 24% alphas
- 066 initial nucleosynthesis combines 3 alphas into carbon 12 simultaneously, very rare
- 067-72 stellar carbon synthesis
072-73 CNO cycle
074-75 Supernova nucleosynthesis
075-76 N14+n makesCarbon 14, half life 5730 years
076-77 isotope ratios ( lead, rubidium, strontium ) -> 3.8GY rocks, 4.6GY meteorites
- 081 neutrons from U-235 fission breed U238 into Pu238
- 085 tonne of spent nuclear fuel produces 100g americium and 20 grams curium
- 087 Arguments about element names
- 087 Possible island of stability for element 126 (Oganesson 118 heaviest discovered)
- 088 Neutron stars may have very heavy elements
- 091 r-process supernovae may produce atomic weight 270
093 Halo nuclei such as He6, Be11, Li11
095 Hypernuclei
096 Strange matter
098 Antimatter- antihydrogen, antideuterium, antihelium
estimated cost $25B for one gram of antimater
- 106 forensics via induced radioactivity: overpainted art, nitrogen in explosives, arsenic in Napoleon's hair
110 (nuclear) Magnetic resonance imaging
Note, reference Nuclear Power A.V.S.I. by Maxwell Irvine 2011 online at Internet Archive Digital Library. Some about plasma fusion physics, but not much help calculating fusion cross section.