Nuclear Systematics Part III: The Source of Solar Luminosity

Author

Oliver Manuel, Missouri University of Science and TechnologyFollow
Cynthia Pearl Bolon, Missouri University of Science and TechnologyFollow
M. Zhong

Abstract

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.

Recommended Citation

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

Department(s)

Chemistry

Keywords and Phrases

Article; Light Exposure; Luminance; Neutron; Nuclear Physics; Solar Energy; Sun

International Standard Serial Number (ISSN)

0236-5731

Document Type

Article - Journal

Document Version

Citation

File Type

text

Language(s)

English

Rights

© 2002 Springer Verlag, All rights reserved.

Publication Date

01 Apr 2002