AAS 199th meeting, Washington, DC, January 2002
Session 146. Our Favorite Star
Oral, Thursday, January 10, 2002, 10:00-11:30am, Georgetown East

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[146.02] Repulsion and Attraction between Nucleons: Sources of Energy for an Iron-rich Sun and for First Generation Stars

C. Bolon (U. Missouri-Rolla)

The nuclear energy surface defined by 3000 stable and radioactive isotopes indicates repulsion between like nucleons (neutral pion exchange) and attraction of unlike nucleons (charged pion exchange). Excluding Coulomb interactions, repulsive n-n and p-p forces appear to be symmetric and weaker than attractive n-p forces. Nuclear stability results mostly from these interactions and Coulomb repulsion (Manuel & Bolon, 2001, J. Radioanal. Nucl. Chem., in press).

Fusion and attractive interactions have long been recognized as probable sources of energy for first generation stars. Dissociation and repulsive nucleon interactions may be sources of energy for the proposed Sun and other second generation stars that may have formed on collapsed cores (neutron stars) of first generation stars (Manuel et al., 2000, J. Fusion Energy 19, 93).

Thus, solar luminosity and solar wind protons may arise from: a) Neutron emission from the central neutron star (NS), b) Neutron decay or capture by other nuclides, c) Fusion as H+ migrates through material accreted on the NS, and d) Escape of H+ in the solar wind.

This scenario (Manuel et al., 2001, 32nd LPSC, abstract 1041) fits the solar neutrino flux (Davis et al., 1968 Phys. Rev. Lett. 20, 1205), neutrino oscillation measurements (Boehm et al., 2000, Phys. Rev. Lett. 84, 3764), light isotope enrichment in the solar wind (Manuel & Hwaung, 1983, Meteoritics 18, 209 ), and excess heavy elements (Reames, 2000, Ap. J. 540, L111) and heavy isotopes (Rao et al., 1991, JGR 96, 19321) in solar flares. The formation of an iron-rich Sun from highly evolved nuclides in the central region of SN debris (Manuel & Sabu, 1977, Science 195, 208) is also consistent with the presence of decay products from short-lived nuclides and inter-linked chemical and isotopic heterogeneities from nucleosynthesis in meteorites and planets.

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The author(s) of this abstract have provided an email address for comments about the abstract: cbolon@umr.edu

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