=== 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  [[ https://en.wikipedia.org/wiki/Patrick_Blackett | Patrick Blackett ]] 1921-4 23,000 cloud chamber photographs of alphas bombarding nitrogen, eight examples of proton ejection and an oxygen 
 .p19 [[ https://en.wikipedia.org/wiki/James_Chadwick | Chadwick ]] neutron 1932
 .p23 [[ https://en.wikipedia.org/w/index.php?title=Special:Search&search=Wolfgang+Pauli&wprov=acrw1_0 | Pauli ]] hypothesized neutrino 1931
  . proton, neutron, electron, neutrino spin 1/2 
 .p25[[ https://en.wikipedia.org/wiki/Ir%C3%A8ne_Joliot-Curie | Joliot-Curie ]]s 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 [[ https://en.wikipedia.org/wiki/Otto_Hahn | Hahn ]] and [[ https://en.wikipedia.org/wiki/Fritz_Strassmann | Strassmann ]] fission 1938, Fermi slow neutrons with paraffin or water so they don't shatter nuclei
 .027 [[ https://en.wikipedia.org/wiki/Lise_Meitner | Lisa Meitner ]] and [[ https://en.wikipedia.org/wiki/Otto_Robert_Frisch | Otto Frisch ]] liquid drop model, instability, fission
 .028 Planck law E=hv
 .032 [[ https://en.wikipedia.org/wiki/Strong_interaction | Strong force ]], neutron stability in nucleus
 .036  [[ https://en.wikipedia.org/wiki/Pion | 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 [[ https://en.wikipedia.org/wiki/Quark%E2%80%93gluon_plasma | Quark-gluon plasma ]] beginning universe
 .041 [[ https://en.wikipedia.org/wiki/Relativistic_Heavy_Ion_Collider | Relativistic Heavy Ion Collider ]] gold or lead atoms, 50x density compared to cold nuclei
 .041 [[ https://en.wikipedia.org/wiki/Blue_Riband | Blue Riband ]]
 .045 [[ https://en.wikipedia.org/wiki/Magic_number_(physics) | 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 [[ https://en.wikipedia.org/wiki/Technetium | Technetium ]] lightest unstable element, τεχνητός =artificial
 .059 [[ https://en.wikipedia.org/wiki/Technetium_star | 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 [[ https://en.wikipedia.org/wiki/CNO_cycle | CNO cycle ]] 
 .074-75 [[ https://en.wikipedia.org/wiki/Supernova_nucleosynthesis | Supernova nucleosynthesis ]]
 .075-76 N14+n makes[[ https://en.wikipedia.org/wiki/Carbon-14  | Carbon 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 [[ https://en.wikipedia.org/wiki/Halo_nucleus | Halo nuclei ]] such as He6, Be11, Li11
 .094 Borromean [[ https://en.wikipedia.org/wiki/Borromean_rings | rings ]]  [[ https://en.wikipedia.org/wiki/Borromean_nucleus | nuclei ]]
 .095 [[ https://en.wikipedia.org/wiki/Hypernucleus | Hypernuclei ]] 
 .096 [[ https://en.wikipedia.org/wiki/Strange_matter | Strange matter ]]
 .098  [[ https://en.wikipedia.org/wiki/Antimatter | Antimatter ]]- antihydrogen, antideuterium, antihelium 
  . estimated cost [[ https://en.wikipedia.org/wiki/Antimatter#Cost | $25B ]] for one gram of antimater
 .106 forensics via induced radioactivity: overpainted art, nitrogen in explosives, arsenic in Napoleon's hair
 .109 [[ https://en.wikipedia.org/wiki/Rutherford_backscattering_spectrometry | Rutherford backscattering spectroscopy ]]
 .109 [[ https://en.wikipedia.org/wiki/Particle-induced_X-ray_emission | Particle-induced X-ray emission  PIXE ]]
 .110 (nuclear) [[ https://en.wikipedia.org/wiki/Magnetic_resonance_imaging | Magnetic resonance imaging ]]
 .112 [[ https://en.wikipedia.org/wiki/Positron_emission_tomography | Positron emission tomography ]]

Note, reference [[ https://archive.org/details/nuclearpowervery0000irvi/mode/2up | 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.