III. Conclusions, Related Observations, and Remaining Problems

Historical Info     Evidence     Conclusions

  The solar neutrino flux has been a long-standing puzzle [1] for the H-filled Sun.   The above observations confirm that it is now obsolete.   On the other hand, a Fe-rich Sun from SN debris offers a direct explanation for these observations and for a) heterogeneous accretion of terrestrial planets [2-4], b) primordial He and radiogenic Xe-129 retained inside the Earth today [5,6] c) non-magmatic iron meteorites [7, pp. 385-406**], d) isotopic anomalies and decay products of short-lived nuclides in iron [pp. 385-406] as well as in primitive [** See pp361-384] meteorites [8], e) the iron gradient in planets and in the planetary system [pp. 608-611], and a) experimental affirmation [9] of all three tests originally proposed for mass fractionation in the Sun [10].

  Two of three major objections to the Fe-Sun have been resolved and a third is in progress.   The discovery [11,12] of pulsar planets confirmed that planetary systems can form directly from SN debris [13].   The Hubble telescope verified the existence of axial ejections from SNs [pp. 241-249].   Extrapolations of trends from the cradle of the nuclides book cover [7] indicate an inherent instability in assemblages of neutrons that may explain solar luminosity and the solar neutrino flux [14,15].   After correcting for fractionation, solar abundances generally correlate with nuclear stability [15], as Harkins had predicted [16], except for a large excess of H-1.   This anomalous H-1 and the outflow of H+ ions in the solar wind may be by-products of solar luminosity [14,15,17-19]
  **All page numbers in brackets [ ] are in ref. 7, Proceedings of the 1999 symposium organized by Glenn T. Seaborg and Oliver K. Manuel. See http://www.wkap.nl/book.htm/0-306-46562-0

References: [1] Bahcall J.N. & Davis R., Jr. (1976) Science 191, 264-267; [2] Eucken A. (1944) Nachr. d. Akad. d. Wiss. Göttingen, Math-Phys. 1, 1-25; [3] Turekian K.K. & Clark S.P., Jr. (1969) Earth Planet. Sci. Lett. 6, 346-348; [4] Vinogradov A.P. (1975) Geokhimiya 10, 1427-1431; [5] Boulos M.S. & Manuel O.K. (1971) Science 174, 1334-1336; [6] Manuel O.K. & Sabu D.D. (1981) Geochem. J. 15, 245-267; [7] Origin of Elements in the Solar Sysyem: Implications of Post-1957 Observations, Proceedings of the 1999 ACS symposium organized by Glenn T. Seaborg and Oliver K. Manuel (Kluwer Academic/Plenum Publishers, New York, NY, USA ed., O.K.Manuel 2000), 646 pp.; [8] Alexander E.C., Jr. & Manuel O.K. (1968) Earth Planet. Sci. Lett. 4, 113-117; [9] Manuel O.K. (1998) Meteoritics 33 (Supplement) A97; [10] Manuel O.K. & Hwaung G. (1983) Meteoritics 18, 209-222; [11] Wolszczan A. & Frail D.A. (1992) Nature 355, 145-147; [12] Wolszczan A.: 1994, Science 264, 538-542; [13] Lin, D.N.C., Woosley, S.E., Bodenheimer, P.H.: 1991, Nature 353, 827-831; [14] Manuel O., Bolon, C., Katragada A. & Insall M. (2000) J. Fusion Energy 19, 93-98; [15] Manuel O., Bolon C., Zhong M. & Jangam P. (2001) Lunar and Planetary Sci. Conf. XXXII, abstract #1041, LPI No. 1080, ISSN No. 0161-5297; [16] Harkins W.D. (1917) J. Am. Chem. Soc. 39, 856-879; [17] Manuel O. & Bolon C. (2002) J. Radioanal. Nucl. Chem. 251, ms. #5391 in press, 13 pp.; [18] Manuel O., Bolon C. & Jangam P. (2002) J. Radioanal. Nucl. Chem. 251, ms. #5415 in press; 17 pp.; [19] Manuel O., Bolon C. & Zhong M. (2002) J. Radioanal. Nucl. Chem. 251, ms. #5401 in press 17 pp.