Other
Scientific paper
Jul 1993
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993metic..28r.348f&link_type=abstract
Meteoritics, vol. 28, no. 3, volume 28, page 348
Other
Accelerator Mass Spectrometry, Budulan, Calcium-41, Cosmic Rays, Estherville, Mesosiderites, Nickel-59
Scientific paper
The cosmogenic radionuclide ^59Ni (t(sub)1/2 = 76 ky) has great potential as a monitor of thermal neutrons in metal-rich extraterrestrial materials. In deep samples from larger meteoroids (which can support a big neutron flux) containing >1% or so of nickel, thermal neutron capture on ^58Ni (sigma(sub)th = 4.6 b) is the dominant production mechanism. Near the surface of mm-size bodies production occurs via primary proton, fast neutron, and alpha reaction channels on Fe, Co, and Ni. We have applied AMS to the measurement of ^59Ni activities (see ref [1] for details) in four samples from the metal phase of the mesosiderites Estherville (fall, 1879) and Budulan, a find. The activities range from 1.5 to 3.5 dpm/g-Ni. Related work is described in refs. [2,3]. To discuss neutron fluxes in Budulan, we must correct the measured ^59Ni activities for terrestrial age. By using measured ^41Ca activities (13-19 dpm/kg-Fe [4]) and a maximum production rate, P(sub)Fe(^41Ca), in stony irons of 21 dpm/kg-Fe [5] we deduce a maximum terrestrial age of 35 ky. After correction for this terrestrial age and normalization to L-chondritic composition [6], the production rates of ^59Ni, P(sub)Fe(^59Ni), range from 5-13 dpm/g-Ni; these values are 2-3 times greater than those reported in [7] for large irons and ~10 times those for chondrites. References [4,8] present ^41Ca data in the silicate and metal phases from the same Estherville and Budulan samples. If thermal neutron production were solely responsible for P(sub)Fe(^59Ni) and P(sub)Sil(^41Ca) (the latter corrected for spallation of oxidized iron in pyroxene), then the thermal neutron fluxes, phi, inferred from each nuclide in a sample should be the same. We deduce ratios of phi(^59Ni)/phi(^41Ca) that range from 0.75 to 1.65. Differences in epithermal yields can account for only a minor fraction of this variation as the ratio of the total resonant neutron absorption integrals for ^40Ca and ^58Ni is within 10% of the ratio of the thermal neutron cross-sections alone. A twofold change in Budulan's terrestrial age alters the flux ratio by 10% at most. Like ^41Ca [9,10], P(sub)Fe(^59Ni) can be used to estimate shielding depths and lower limits on the pre-atmospheric radius. Calculations by [11] give a maximum value for P(sub)Fe(^59Ni) of 22 atoms/min/g-Ni at the center of an L-chondrite with a radius of 300 g/cm^2. The ^10Be and ^26Al activities in Estherville [5] and respective semi-empirical production rate formulas [12] set a maximum meteoroid radius of 300 g/cm^2. Our measured value for ^59Ni implies a lower radius limit of 150 g/cm^2 and shielding depths of 60-150 g/cm^2. Similarly for Budulan, we suggest a radius of 200 < R < 400 g/cm^2 and shielding depths from 40-200 g/cm^2. We infer that the above samples originated at relatively large depths (except for perhaps Budulan-2428) in meteoroids with preatmospheric radii > 30 cm, assuming a mesosiderite density of 5.5 g/cm^3. Interestingly, those samples (Budulan-2357 and Estherville-3311) having ^41Ca production rates that indicate a higher degree of shielding, have flux ratios equal to or less than 1; the other two samples have ^41Ca contents typical of near-surface exposure and have ratios phi(^59Ni)/phi(^41Ca) larger than unity. This correlation indicates that P(sub)59 from fast neutron reactions on ^60,61Ni enhances ^59Ni production at near surface regions. References: [1] Paul M. et al. (1993) Nucl. Inst. Meth., submitted. [2] Kutschera W. et al. (1992) Nucl. Inst. Meth., in press. [3] Klein J. et al.(1993) Meteoritics (this issue). [4] Albrecht A. et al. (1992) LPS XXIII, 5-6. [5] Vogt S. et al. (1991) Meteoritics, 26, 403. [6] Fink D. et al.(1992) LPS XXIII, 355-356. [7] Honda et al. (1967) Handb. Physik. 46(2), 613-632. [8] Fink D. et al. (1991) EPSL, 107, 115-128. [9] Fink D. et al. (1990) Nucl. Inst. Meth., B47, 79-96. [10] Klein J. et al. (1991) Meteoritics, 26, 358. [11] Spergel M. et al.(1986) Proc. LPS 16th; J. Geophys. Res., 91, D483-D494. [12] Graf et al. (1992) GCA, 54, 2521-2534.
Albrecht Andreas
Allan G. L.
Fifield Keith L.
Fink David
Herzog Gregory F.
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