Binding energies of Q-nuclei and stellar hydrogen burning

Details Binding energies of Q-nuclei and stellar hydrogen burning Binding energies of Q-nuclei and stellar hydrogen burning

Dec 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986apj...311..485h&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 311, Dec. 1, 1986, p. 485-490.

Astronomy and Astrophysics

Astrophysics

3

Hydrogen, Nuclear Astrophysics, Nuclear Binding Energy, Nuclear Fusion, Solar Neutrinos, Stellar Physics, Hadrons, Particle Mass, Quarks

Scientific paper

Nuclear structural aspects of the possibility that a Q-nuclear cycle could exist with the inclusion of a quark-stabilized A = 5 nucleus are studied in detail. Using a realistic nucleon-nucleon interaction to produce saturation in normal nuclei, a quark-nucleon interaction based on the one-pion exchange potential, and a full-scale shell-model diagonalization in the 1s, 1p shell, including all Coulomb effects, the authors find that a stable A = 5 cycle is possible which does exhibit many of the expected features, such as shrinkage of the quarked nuclei as compared with normal nuclei. However, it is also found that the cycle is constrained to produce beta(+) endpoint energies, which would lead to fluxes of high-energy neutrinos orders of magnitude too large to be consistent with the known limits. The required quarked nucleus concentration is also orders of magnitude larger than present estimates based on experiment and theory. It is concluded the the Q-nuclear cycle is not likely to be a solution to the solar neutrino problem.

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