Photodisintegration

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Photodisintegration (also called phototransmutation) is a nuclear process in which an atomic nucleus absorbs a high-energy gamma ray, enters an excited state, and immediately decays by emitting a subatomic particle. The incoming gamma ray effectively knocks one or more neutrons, protons, or an alpha particle out of the nucleus.[1] The reactions are called (γ,n), (γ,p), and (γ,α).

Photodisintegration is endothermic (energy absorbing) for atomic nuclei lighter than iron and sometimes exothermic (energy releasing) for atomic nuclei heavier than iron. Photodisintegration is responsible for the nucleosynthesis of at least some heavy, proton-rich elements via the p-process in supernovae.

Photodisintegration of deuterium[edit]

A photon carrying 2.22 MeV or more energy can photodisintegrate an atom of deuterium:

2
1
D
 

γ
 
→  1
1
H
 

n

James Chadwick and Maurice Goldhaber used this reaction to measure the proton-neutron mass difference.[2] This experiment proves that a neutron is not a bound state of a proton and an electron,[3] as had been proposed by Ernest Rutherford.

Photodisintegration of beryllium[edit]

A photon carrying 1.67 MeV or more energy can photodisintegrate an atom of beryllium-9 (100% of natural beryllium, its only stable isotope):

9
4
Be
(γ,n) 2α

Antimony-124 is assembled with beryllium to make laboratory neutron sources and startup neutron sources. Antimony-124 (half-life 60.20 days) emits β− and 1.690MeV gamma rays (also 0.602MeV and 9 fainter emissions from 0.645 to 2.090 MeV), yielding stable tellurium-124. Gamma rays from Antimony-124 knock neutrons off beryllium-9 with an average kinetic energy of 24keV, intermediate neutrons. The other product is two alpha particles.[4][5]

Other isotopes have higher thresholds for photoneutron production, as high as 18.72 MeV, for carbon-12.[6]

Hypernovae[edit]

In explosions of very large stars (250 or more times the mass of the Sun), such as pair-instability supernovae, photodisintegration is a major factor in the supernova event. As the star reaches the end of its life, it reaches temperatures and pressures where photodisintegration's energy-absorbing effects temporarily reduce pressure and temperature within the star's core. This causes the core to start to collapse as energy is taken away by photodisintegration, and the collapsing core leads to the formation of a black hole. A portion of mass escapes in the form of relativistic jets, which could have "sprayed" the first metals into the universe.[7][8]

Photofission[edit]

Photofission is a similar but distinct process, in which a nucleus, after absorbing a gamma ray, undergoes nuclear fission (splits into two fragments of nearly equal mass).

See also[edit]

Pair-instability supernova

References[edit]

  1. ^ Clayton, D. D. (1984). Principles of Stellar Evolution and Nucleosynthesis. University of Chicago Press. p. 519. ISBN 978-0-22-610953-4. 
  2. ^ Chadwick, J.; Goldhaber, M. (1934). "A nuclear 'photo-effect': disintegration of the diplon by γ rays". Nature. 134 (3381): 237–238. Bibcode:1934Natur.134..237C. doi:10.1038/134237a0. 
  3. ^ Livesy, D. L. (1966). Atomic and Nuclear Physics. Waltham, MA: Blaisdell. p. 347. LCCN 65017961. 
  4. ^ Lalovic, M.; Werle, H. (1970). "The energy distribution of antimonyberyllium photoneutrons". Journal of Nuclear Energy. 24 (3): 123–132. Bibcode:1970JNuE...24..123L. doi:10.1016/0022-3107(70)90058-4. 
  5. ^ Ahmed, S. N. (2007). Physics and Engineering of Radiation Detection. p. 51. ISBN 978-0-12-045581-2. 
  6. ^ Handbook on Photonuclear Data for Applications: Cross-sections and Spectra. IAEA. 
  7. ^ Fryer, C. L.; Woosley, S. E.; Heger, A. (2001). "Pair-Instability Supernovae, Gravity Waves, and Gamma-Ray Transients". The Astrophysical Journal. 550 (1): 372–382. Bibcode:2001ApJ...550..372F. arXiv:astro-ph/0007176Freely accessible. doi:10.1086/319719. 
  8. ^ Heger, A.; Fryer, C. L.; Woosley, S. E.; Langer, N.; Hartmann, D. H. (2003). "How Massive Single Stars End Their Life". The Astrophysical Journal. 591 (1): 288–300. Bibcode:2003ApJ...591..288H. arXiv:astro-ph/0212469Freely accessible. doi:10.1086/375341.