Chemical and isotopic compositions of meteorites, the solar wind, solar flares, and planets provide evidence for local synthesis of the chemical elements and formation of the solar system from heterogeneous debris of a supernova that exploded axially [1], as shown in Fig 1. Such explosions produce the bipolar nebulae recently seen with the Hubble telescope [2].

Fig. 1 is a more viable explanation for isotopic anomalies and short-lived radioactivities in meteorites than addition of 10^-4 parts of exotic nucleogenetic material to 0.9999 parts normal solar system material [3,4] and offers a natural mechanism for properties (a-j) of the sun, its planetary system and other stellar objects that are unexplained by exotic additions:

a) Chemical stratification of the planetary nebula [5]
b) Heterogeneous accretion of the terrestrial planets [6]
c) Interlinked chemical and isotopic heterogeneities in the nebula [7]
d) "Mirror-image" isotopic anomalies in meteorites [8]
e) Grain-size dependent levels of extinct ²⁶Al in meteorites [9]
f) Grain-size dependent isotopic anomalies in meteorites [10]
g) Diffusive enrichment of hydrogen and lighter isotopes of other elements at the solar surface [11,12]
h) Disruption of intrasolar diffusion to produce less anomalous isotope ratios in solar flare particles [13]
i) Planets orbiting a collapsed supernova core, PSR 1257+12 [14]
j) The formation of planets in a rotationally-supported disk of super nova debris that orbits the collapsed supernova core [15]

Fig. 1. Heterogeneous debris of a supernova produced the solar system [1]

References: [1] Oliver L. L, Ballad R. V., Richardson J. F. and Manuel O. K. (1981) J. Inorg. Nucl. Chem. 43, 2207-2216. [2] Frank A. (1997) Astronomy, February issue, 36- 43. [3] Fowler W. A. (1984) Science 226, 922-935. [4] Wasserburg G. J. (1987) Earth. Planet. Sci. Lett. 86, 129-173. [5] Ringwood A. E. (1989) Earth. Planet. Sci. Lett. 95, 1-7. [6] Turekian K. K. and Clark S. P. (1969) Earth. Planet. Sci. Lett. 95, 346-348. [7] Lee J. T., Li Bin and Manuel O. K. (1997) Comments Astrophys. 18, 335-345. [8] Begemann F. (1993) in Origins and Evolution of the Elements (eds., N. Prantzos, E. Vangioni-Flam and M. Casse) pp. 518-527, Cambridge University Press, Cambridge. [9] Kuroda P. K. and Meyers W. A. (1997) Radiochim. Acta, in press. [10] Amari S., Zinner E. and Lewis R. S. (1996) Lunar Planet. Sci. 27, 23-24. [11] Manuel O. K. and Hwaung G. (1983) Meteoritics 18, 209-222. [12] MacElroy J. M. D. and Manuel O. K. (1986) J. Geophys. Res. 91, D473-D482. [13] Rao M. N. et al. (1991) J. Geophys. Res. Space Phys. 96, 19321-19330. [14] Wolszczan A. and Frail D. A. (1992) Nature 355, 145-147; Wolszczan A. (1994) Science 264, 538-542. [15] Lin D. N. C., Woosley S. E. and Bodenheimer P. H. (1991) Nature 353, 827-829.

This paper is dedicated to the memory of Dr. Dwarka Das Sabu.