Neutron capture

Neutron capture is a nuclear reaction in which an atomic nucleus and one or more neutrons collide and merge to form a heavier nucleus.^[1] Since neutrons have no electric charge, they can enter a nucleus more easily than positively charged protons, which are repelled electrostatically.^[1]

Neutron capture plays a significant role in the cosmic nucleosynthesis of heavy elements. In stars it can proceed in two ways: as a rapid process (r-process) or a slow process (s-process).^[1] Nuclei of masses greater than 56 cannot be formed by thermonuclear reactions (i.e., by nuclear fusion) but can be formed by neutron capture.^[1] Neutron capture on protons yields a line at 2.223 MeV predicted^[2] and commonly observed^[3] in solar flares.

^ ^a ^b ^c ^d Ahmad, Ishfaq; Hans Mes; Jacques Hebert (1966). "Progress of theoretical physics: Resonance in the Nucleus". Institute of Physics. 3 (3): 556–600.
^ Morrison, P. (1958). "On gamma-ray astronomy". Il Nuovo Cimento. 7 (6): 858–865. Bibcode:1958NCim....7..858M. doi:10.1007/BF02745590. S2CID 121118803.
^ Chupp, E.; et al. (1973). "Solar Gamma Ray and Neutron Observations". NASA Special Publication. 342: 285. Bibcode:1973NASSP.342..285C.

[University_of_Ottawa_(Department_of_Physics)-1] Ahmad, Ishfaq; Hans Mes; Jacques Hebert (1966). "Progress of theoretical physics: Resonance in the Nucleus". Institute of Physics. 3 (3): 556–600.

[2] Morrison, P. (1958). "On gamma-ray astronomy". Il Nuovo Cimento. 7 (6): 858–865. Bibcode:1958NCim....7..858M. doi:10.1007/BF02745590. S2CID 121118803.

[3] Chupp, E.; et al. (1973). "Solar Gamma Ray and Neutron Observations". NASA Special Publication. 342: 285. Bibcode:1973NASSP.342..285C.

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