Nuclear Systematics Part III: The Source of Solar Luminosity
The Sun emits about 3·10431H per year in the solar wind (SW). Solar luminosity and the outflow of SW-protons come from the collapsed supernova core. a neutron star (NS), on which the Sun formed. The universal cradle of the nuclides indicates that the energy of each neutron in the Sun's central NS exceeds that of a free neutron by ≈10-22 MeV. Solar luminosity and SW-protons are generated by a series of reactions: (a) escape of neutrons from the central NS, (b) decay of free neutrons or their capture by heavier nuclides, (c) fusion and upward migration of H+ through material that accreted on the NS, and (d) escape of H+ in the SW.
O. Manuel et al., "Nuclear Systematics Part III: The Source of Solar Luminosity," Journal of Radioanalytical and Nuclear Chemistry, vol. 252, pp. 3-7, Springer Verlag, Apr 2002.
The definitive version is available at https://doi.org/10.1023/A:1015255732525
Keywords and Phrases
Article; Light Exposure; Luminance; Neutron; Nuclear Physics; Solar Energy; Sun
International Standard Serial Number (ISSN)
Article - Journal
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