some of the well-established symmetries in the universe may have to be abandoned .In about 1930 it was noticed that when a proton passed closer than about 1 .4 fmto the nucleus of an atom, it was attracted to it, rather the repelled, an Coulomb' slaw would suggest . However, when two protons actually carne into contact, they werenaturally repelled, because of the 'exclusion Principle . It was already accepted tha telectromagnetic forces were caused by the exchange of massless quanta, photons ,between <strong>particles</strong> . As we can see from looking at the binding energies of differen tnuclei on a Periodic Table, these are all roughly the same, and equal to 8 HeV ,whereas the ionization potentials of different elements are very irregular . Thi ssuggests that the nuclear force, which is responsible for holding nuclei together i s'saturated', unlike the Coulomb force, and this fact led Heisenberg to propose, i n1932, that the nuclear force was a so-called 'exchange force' . An exchange force i sone in which the properties of the <strong>particles</strong> interacting through it are exchanged .For this reason, it cannot be represented simply by a simple potential V(r), but onlyby the product PayV(r), where P is the so-called 'permutation operator' and a and bare the <strong>particles</strong> taking part in the reaction . Thus, if the wave function of the pai rof interacting <strong>particles</strong> is O)f(a,b), we see tha tP o 67~ (a, b ) _ '1'c( b , a ) .Before we discuss the nature of the strong nuclear force in any greater detail, le tus first consider how H .Yukawa managed to make his startling predictions about it squanta in 1935 . Yukawa reasoned that, because of the very short range of the nuclea rforce, its quanta must be comparatively massive . But, if this were the case, how wa sit that mass fluctuations were not observed in protons and neutrons? The only answe rto this question was that the emission and reabsorbtion of quanta took place in tooshort a time for the Uncertainty Principle to allow one to observe . Invoking the time -energy uncertainty relation we then havemt
were looking for, experimenters set out to try and find Yukawa's quanta .It was postulated that, just asphotons are released when charged <strong>particles</strong> collide ,so Yukawa's new quanta would be produced when nucleons collided . But the only plac ewhere sufficiently energetic collisions could occur was in cosmic rays . Thus, in 1936 ,extensive research on cosmic ray <strong>particles</strong> began . Most of the research was done usingcloud chambers . experimenters measured the radius of curvature and lengths of track sobtained in these, and could thus calculate the mass of the particle which ha dproduced them . Late in 1936, while doing research at mountain altitudes, C .Anderson andS .Neddermeyer found the tracks of a new particle having a mass of around 106 I4eV i ntheir cloud chamber. They named this particle a 'mesotron' and this word was soo nshortened to meson . After a short gap in research caused by the war, further test swere carried out on these newly-detected <strong>particles</strong> . It was found that they could bedetected at sea-level and even in deep mines, suggesting that they did not interactwith atomic nuclei nearly as much as Yukawa's mesons should . It was suggested tha tthe new <strong>particles</strong> formed the hard component of cosmic rays . It was discovered that layersof lead appeared to stop less of these new <strong>particles</strong> than did the air, and so it wa sconcluded that the <strong>particles</strong> were unstable, and integration of a large number o fresults yielded a mean lifetime of 2 microseconds . A direct method to determine th elifetime of the new meson was employed by Hasetti . He had four counters, two aboveand two below, a 10 cms thick iron absorber . Mesons which stopped in the iron, asrecorded by the anticoincidence of the second set of counters with the first set ,tended, after a period of about 2 yAs to emit another charged <strong>particles</strong> which wa sdetected by the second two counters .Doubts began to grow as to whether the new meson was in fact Yukawa's meson . I thad the right mass, but it did not interact sufficiently with atomic nuclei . In 194 7Conversi, Pancini, and Piccioni obtained more concrete evidence that this was not th eYukawa meson . They studied the absorption of negative mesons by blocks of iron an dcarbon . It was found that the absorption rate was directly proportional to the atomi cnumber, and in carbon, where Z=12, about half the mesons were c ap tured, indicatin gan average capture time of 1)es . The process of meson capture is that the meson i scaptured by an atom and goes into an electron-type orbit, and quickly cascades downto the lowest possible orbit, about two hundred times as close to the nucleus for ameson as for an electron, because of its greater mass . Thus, any particle whichinteracts with nucleons will be absorbed by the nucleus in about 1 0-1 ; s, the characteristictime of the strong nuclear reaction . But the newly-found meson were takin gabout 10 '7 times too long to react with atomic nuclei, and so it was concluded tha tthey were not the <strong>particles</strong> predicted by Yukawa .Later in 1947, Bethe and Marshak suggested that there must be another meson whic hcorresponded to Yukawa's particle, and at the end of 1947, Lattes, Luirhead, Ochialini ,and Powell observed the decay of a very short-lived meson into another meson i nphotographic emulsion . When many tracks of this type had been produced by flyin gemulsions at high altitudes in balloons, it was seen that an initial particle of mas saround 140 MeV decayed into a second particle of mass 100 '1deV, which itself eventuall ydecayed into an electron . It has been found that the first particle in this chain i sthe pion, which fits very well with Yukawa's predictions, and the second is the muon .As we have seen, crude measurements were made of pion and muon properties in earl ywork with cosmic rays, but it was obvious that much more precise measurements would b epossible if the <strong>particles</strong> were to be produced artificially . It was calculated that th ethreshold energy for the production of charged pions from the collision of two nucleons
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- Page 55 and 56: is 1 .3 x 10 s . The leaders o; is,
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photon, .4•*l, and for the antiph
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should expect some asymmetry in the
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p where L is the orbital momentum o
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about 70°' of the ne utrons . Afte
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We consider an isolated system of n
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on their spins . We find that if we
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device : scalers, which record the
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In appearance, semiconductor partic
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Usually, photons passing through a
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during this short time, worthwhile
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CHAPTER NINE: THE ACCELERATION OF P
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1931 Sloan and Lawrence built a thi
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faster than light . instead, the ph
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employed for each function . In act
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and again by Budker and Veksler in
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BIBLIOGRAPHY .General works :The Ph
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Scalar : .esons may ihplain by the
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Name S J I I s U P GY ND ND 1 ND ND
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p5,55' 77 6570p 070601,.635 67.7355
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A .3 Quark combinations to fora sta
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s+ki # 13 .41M.V I9mo. dxry nvla)33
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k.1515e.pr rim
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° Prix.-.,a..u(14751 o IMfon.ly ca
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A .5 Conservation and invariance la
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F_AG Fixed field alternating gradie
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S Scalar gamma matrix product .S En
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Elastic cross—section .Inelastic
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C .3 Compound SI units used in this
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w oE >< k)- c; ev--o ;,o»,--.@r«-
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APPENDIX F : PHYSICAL CONSTANTS .(F