Collateral consequences of the inhomogeneous distribution of short-lived radionuclides in the solar nebula

Details Collateral consequences of the inhomogeneous distribution of short-lived radionuclides in the solar nebula Collateral consequences of the inhomogeneous distribution of short-lived radionuclides in the solar nebula

Nov 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999m%26ps...34..869n&link_type=abstract

Meteoritics & Planetary Science, vol. 34, no. 6, pp. 869-884 (1999).

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Scientific paper

The presence of several short-lived (now extinct) radionuclides in the early solar system demands that they were synthesized and added to preexisting solar system materials shortly (on a time scale of the order of the relevant radionuclide lifetime) before formation of solar system solids. For diverse reasons it is often suggested that the solar system distributions of these radionuclides were radically heterogeneous, perhaps because of the late addition. Much attention has been given to the astrophysical circumstances that might govern the synthesis and distribution of these short-lived radionuclides, but comparatively little attention has been devoted to the distribution of co-synthesized isotopes. The focus of this paper is a systematic, quantitative evaluation of the collateral consequences in stable and long-lived isotopes which might be expected if short-lived radionuclides, in particular 26Al or 53Mn, were injected at their canonical levels and inhomogeneously distributed in the early solar system. We mix model massive star yields of Meyer et al. (1995) and Woosley and Weaver (1995) into a reservoir of cosmic composition, as tabulated by Anders and Grevesse (1989). To mitigate the effects of systematic deviations that may be present in these mixtures due to uncertainties in model stellar yields, we follow Timmes and Clayton (1996) and also mix into a "renormalized" proxy solar system composition computed from a galactic chemical evolution model based primarily on the stellar yields of Woosley and Weaver (1995). The results are very unfavorable to the likelihood of heterogeneously distributed 26Al derived from supernova ejecta. If a massive star is invoked to account for 26Al, its ejecta must have been rather uniformly distributed, as inferred from the lack of measured collateral anomalies in several elements, notably Ca, Cr and Ni. Conversely, if 26Al were indeed radically heterogeneously distributed, some other nucleosynthetic source, more efficient at producing 26Al, is required. In principle, a similar statement applies to 53Mn, but the situation is more complicated. The inferred anomalies at 53Cr will depend not only on how much 53Mn is added by a heterogeneous component, but also more sensitively on the contributions to the associated stable nuclides, 53Cr, 52Cr and 50Cr. Consideration of predicted collateral anomalies provides no direct support for heterogeneously-distributed supernova-derived 53Mn, but the required quantity of supernova contribution, and thus also the collateral anomalies, are much less for 53Mn than for 26Al. With allowance for model calculation uncertainties, it could be argued that anomalies collateral to heterogeneous 53Mn might be small enough to have evaded detection.

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