An antiproton (symbol p, pronounced p-bar) is the antiparticle of the proton. An antiproton is relatively stable, but it is typically short-lived because any collision with a proton will cause both particles to be annihilated in a burst of energy. It was discovered in 1955 by University of California, Berkeley physicists Emilio Segrè and Owen Chamberlain, for which they were awarded the 1959 Nobel Prize in Physics. At CERN in Geneva, Switzerland, and Fermilab in Batavia, Illinois, antiprotons are routinely produced and used for scientific research.
The quark structure of the proton.
The properties of the antiproton are predicted by CPT symmetry to be exactly related to those of the proton. In particular, CPT symmetry predicts the mass and lifetime of the antiproton to be the same as those of the proton, and the electric charge and magnetic moment of the antiproton to be opposite in sign and equal in magnitude to those of the proton.
In mid-June 2006, scientists at CERN (the European Organization for Nuclear Research, or, in French, Organisation Européenne pour la Recherche Nucléaire) succeeded in determining the mass of the antiproton, which they measured at 1,836.153674(5) times more massive than an electron. This is exactly the same as the mass of a "regular" proton, as predicted. The formation of antimatter is related to questions about what happened around the time of the Big Bang, and why such a small amount of antimatter remains in our Solar System today.
The formation of antiprotons requires energy equivalent to a temperature of ten trillion K (1013 K), which is not attained under most natural conditions. However, at CERN (the European Organization for Nuclear Research, or, in French, Organisation Européenne pour la Recherche Nucléaire), protons are accelerated in the Proton Synchrotron (PS) to an energy of 26 GeV, and then smashed into an iridium rod. The protons bounce off the iridium nuclei with enough energy for matter to be created. A range of particles and antiparticles are formed, and the antiprotons are separated off using magnets in vacuum.
Antiprotons have been detected in cosmic rays for over 25 years, first by balloon-borne experiments and more recently by satellite-based detectors. The standard picture for their presence in cosmic rays is that they are produced in collisions of cosmic ray protons with nuclei in the interstellar medium, via the reaction:
p A → p p p A
The secondary antiprotons (p) then propagate through the galaxy, confined by the galactic magnetic fields. Their energy spectrum is modified by collisions with other atoms in the interstellar medium, and antiprotons can also be lost by "leaking out" of the galaxy.
The antiproton cosmic ray energy spectrum is now measured reliably and is consistent with this standard picture of antiproton production by cosmic ray collisions. This sets upper limits on the number of antiprotons that could be produced in exotic ways, such as from annihilation of supersymmetric dark matter particles in the galaxy, or from the evaporation of primordial black holes. This also provides a lower limit on the antiproton lifetime of about one to ten million years. Since the galactic storage time of antiprotons is about ten million years, an intrinsic decay lifetime would modify the galactic residence time and distort the spectrum of cosmic ray antiprotons. This is significantly more stringent than the best laboratory measurements of the antiproton lifetime:
Recent experiments for antiproton detection in cosmic rays include the following:
Antiprotons are routinely produced at Fermilab for collider physics operations in the Tevatron, where they are collided with protons. The use of antiprotons allows for a higher average energy of collisions between quarks and antiquarks than would be possible in proton-proton collisions. The theoretical basis for this is that the valence quarks in the proton and the valence antiquarks in the antiproton tend to carry the largest fraction of the proton or antiproton's momentum.
All links retrieved April 6, 2016.
|Particles in physics|
|elementary particles||Elementary fermions: Quarks: u · d · s · c · b · t • Leptons: e · μ · τ · νe · νμ · ντ
Elementary bosons: Gauge bosons: γ · g · W± · Z0 • Ghosts
|Composite particles||Hadrons: Baryons(list)/Hyperons/Nucleons: p · n · Δ · Λ · Σ · Ξ · Ω · Ξb • Mesons(list)/Quarkonia: π · K · ρ · J/ψ · Υ
Other: Atomic nucleus • Atoms • Molecules • Positronium
|Hypothetical elementary particles||Superpartners: Axino · Dilatino · Chargino · Gluino · Gravitino · Higgsino · Neutralino · Sfermion · Slepton · Squark
Other: Axion · Dilaton · Goldstone boson · Graviton · Higgs boson · Tachyon · X · Y · W' · Z'
|Hypothetical composite particles||Exotic hadrons: Exotic baryons: Pentaquark • Exotic mesons: Glueball · Tetraquark
Other: Mesonic molecule
|Quasiparticles||Davydov soliton · Exciton · Magnon · Phonon · Plasmon · Polariton · Polaron|
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