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'Spectacle' Halo

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(reprinted from Nature, Vol. 252, No. 5484, pp. 564−566, December 13, 1974)

Polonium radiohaloes occur widely and not infrequently (total about 10¹⁵−l0²⁰) in Precambrian rocks but their existence has so far defied satisfactory explanation based on accepted nucleocosmogeochemical theories¹. Do Po haloes imply that unknown processes were operative during the formative period of the Earth? Is it possible that Po halos in Precambrian rocks represent extinct natural radioactivity² and are therefore of cosmological significance? A detailed comparison between an unusual array of Po halo radiocentres and U−Th halo radiocentres is presented here as bearing on the above questions.

Generally, radiohaloes occur in one of several mineralogical contexts^{1, 3, 4}. First, as single haloes around discrete inclusions well isolated from other mineral defects and haloes; second, as single haloes around discrete inclusions lodged in conduits or cleavage cracks; third, as single haloes randomly spaced in clusters (sometimes overlapping); fourth, as vein haloes which formed from a continuous distribution of radioactivity (apparently deposited from hydrothermal solutions) along a conduit; and fifth, as line haloes, which surround, not conduits or cracks, but genuine single inclusions which are long (for example, 25 μm) compared with their width (perhaps 1 μm). Large, amorphous, coloured regions without discrete inclusions are not haloes.

Fig. 1 'Spectacle' array of 210Po haloes in biotite. Halo radius, 18.5 μm.

A striking exception¹ to this classification is the 'spectacle' coloration pattern (Fig. 1), which exhibits two almost circular rings of inclusions joined by a linear array of inclusions. As far as we know this is unlike any group of haloes previously seen. This geometrical arrangement of halo radiocentres, found in a Precambrian biotite from Silver Crater Mine, Faraday Township, Ontario, exhibits true radiohalo characteristics.

First, the coloration is identical to that of normal haloes found about 300 μm away in the same mica specimen. Second, the three-dimensional nature of the halo pattern was demonstrated when the specimen (initially about 50 μm thick) was cleaved; both halves revealed matching 'spectacle' coloration patterns, the only difference being the presence of the inclusion array in one half and its absence in the other half. Third, the radius of the coloration band (18.5 μm) implied an origin from ²¹⁰Po α decay. Mass spectrometric and X-ray fluorescence methods were used to ascertain whether this was indeed a Po halo array.

Before applying these techniques to the 'spectacle' halo, we established that ion-microprobe mass analyses and scanning electron microscope X-ray fluorescence (SEMXRF) studies of 'normal' or 'standard' halo radiocentres (those formed from both U and Th α decay) yielded data consistent with the visual means of identification. Several U−Th haloes (see, for example, photo insert, Fig. 2) found in a Precambrian pegmatitic mica from Rossi, New York, were analyzed by X-ray and ion-probe techniques. Several U−Th halo radiocentres were chosen which contained only U, Th and Pb in any significant abundance, thereby virtually eliminating any molecular ion interference in the Pb−Th−U region (m/e = 204−238) in the ion probe.

Fig. 2 Ion microprobe and XRF comparison between mica matrix and U−Th halo inclusion.

That the mica matrix⁵ yielded insignificant molecular ion currents in the region m/e 160−320 is evident from the data in the lower portion of Fig. 2. In contrast, the recorded spectra of a U−Th inclusion (upper left portion of Fig. 2) revealed a significant number of ion counts accumulated in 12 passes of the regions m/e 204−209 and (with a different scale) m/e 232−240. Total ion counts are tabulated just above the two spectra. The scans on the Pb−Bi region (m/e 204−209) lasted for several minutes and were taken before the scans (equal time) on the U−Th region.

Exact ²⁰⁶Pb/²³⁸U and ²⁰⁸Pb/²³²Th ratios are not obtainable from the ion count data in Fig. 2 because variable U and Th concentrations were observed as the ion probe beam sputtered away the inclusion; accurate ratios could be obtained by simultaneously accumulating counts in the region 204−238 provided that the greater secondary ion yield of U and Th as compared with Pb is taken into account. On the other hand, the separate Pb and U isotope ratios are meaningful. Note, for example, that after subtraction of background counts at m/e 240 from the total counts at m/e 235 and 238, the 235/238 value (0.76) satisfactorily approximates (considering the relatively small number of counts collected) the natural U isotopic ratio, ²³⁵U/²³⁸U = 0.72. The absence of a peak at 204 shows there is little or no common lead in the inclusion and therefore, that the 206/207 ratio is that of ²⁰⁶Pb/²⁰⁷Pb as derived from in situ U decay.

Also shown in Fig. 2 are the SEMXRF spectra of the mica matrix and the U−Th halo radiocentre, both of which correlate well (with the exception of the low Z and low abundance elements in the former) with the respective ion-probe spectra. Only U, Th and Pb are exclusively in the inclusion.

The ion-microprobe mass spectrum of the mica matrix surrounding the 'spectacle' halo was nearly identical to the mica spectrum shown in Fig. 2 and is not repeated in Fig. 3. Figure 3 (top centre) shows the portion m/e = 160−264 of the ion-microprobe spectrum (verical log scale) of several of the inclusions. Also shown is the actual ion-probe trace of the important region from m/e = 204−210 using a linear vertical scale and an expanded horizontal scale. There is no significant ion current above m/e = 209; that is, no significant ion signals were detected at any of the prominent U and Th peaks: 238(U⁺), 254(UO⁺), 232(Th⁺) and 248(ThO⁺). No m/e = 204 was detected above background (1 c.p.s.), and the 206/207 mass ratio was ≃20 (206 signal ≃2,000 c.p.s.).

Fig. 3 Ion microprobe and SEMXRF spectra of mica matrix and 210Po halo inclusions.

Figure 3 also shows SEMXRF spectra of the surrounding mica and of one of the Po halo radiocentres. Lead is the only element detectable in this radiocentre exclusive of the mica; some adjacent radiocentres revealed Bi as well. The use of two different instruments, and longer counting times, account for the slightly different X-ray spectra in Figs 2 and 3. The excellent resolution of the SEM showed the Pb-rich areas to coincide exactly with the Po halo radiocentres which are visible both in ordinary transmitted (Fig 1) and reflected light microscopy. Regions as close as 1 μm to the radiocentres showed virtually no Pb or Bi, implying little if any diffusion loss from the inclusions.

As the X-ray data definitely show Pb (and sometimes Bi) in the 'spectacle' halo radiocentres, and as there is no evidence for any molecular ion contribution in the region from m/e = 204−238, the 206, 207 and 208 peaks are interpreted as Pb isotopes and 209 as ²⁰⁹Bi. ²⁰⁴Pb, a constituent of both common and primordial Pb, is missing (no 204 peak), implying that the 'spectacle' halo inclusions analyzed contained no detectable Pb of either of these types. Absence of the 232, 235 and 238 peaks is interpreted as showing the inclusions contain virtually no ²³²Th, ²³⁵U or ²³⁸U and, therefore, no radiogenic ²⁰⁸Pb, ²⁰⁷Pb or ²⁰⁶Pb derived from the in situ decay of these isotopes. The 207 and 208 peaks are therefore attributed to ²⁰⁷Pb and ²⁰⁸Pb, perhaps arising from the decay of minute amounts of ²¹¹Bi and ²¹²Bi within the inclusions^5,6. The ²⁰⁹Bi is considered to be primordial.

The outstanding feature of the mass analysis is the prominent 206 signal which, when attributed to the presence of ²⁰⁶Pb in the inclusions, fits perfectly with the prediction based on ring structure measurements, that is, that the ²⁰⁶Pb is radiogenically derived, not from U or Th, but directly from ²¹⁰Po α decay. In this respect, the large difference in the 206/238 (²⁰⁶Pb/²³⁶U) ratio between the 'spectacle' halo and the U−Th halo (Figs 2 and 3) is especially significant. Clearly the 'spectacle' halo resulted from ²¹⁰Po α decay; an explanation for its geometry is still under study.

Because the Pb isotope in these inclusions is not explicable as any combination of common, primordial, or from in situ Pb derived radiogenically in situ from U or Th, we conclude that a different type of Pb, derived from Po α decay, exists in nature. Supportive evidence comes from electron-probe and ion-probe analyses of a ²¹⁸Po halo radiocentre found in a mica from the Iveland District, Norway, which yielded a ²⁰⁶Pb/²⁰⁷Pb ratio of 23. This is consistent with that expected from ²¹⁸Po a decay to ²⁰⁶Pb. Such a Pb ratio is impossibly high based on normal isotopic ²³⁸U/²³⁵U decay, the theoretical maximum being 21.8.

Other investigations have shown varying mixtures of U-derived and Po-derived Pb may occur in the same radiocentre, for there exists an almost continuous halo spectrum stretching from "pure" U to "pure" Po haloes. Only a few (<0.01) Po haloes in biotite may survive the delicate sectioning process necessary for SEM X-ray analysis.

Just as important as the existence of a new type of lead is the question of whether Po haloes which occur in a granitic or pegmatitic environment (for example, in mica, fluorite or cordierite) can be explained by accepted models of Earth history¹. (R. V. G. has found other ²¹⁰Po haloes that differ essentially from those in granites-unpublished information.)

This research has been sponsored by the United States Atomic Energy Commission under contract with Union Carbide Corp. and by Columbia Union College with an assistance grant from the National Science Foundation. Thanks are due to R. I. Gait and J.A. Mandarino, Royal Ontario Museum, Louis Moyd, National Museum of Canada, and G. Switzer, United States National Museum, for providing specimens.

Received July 31, 1974.

References

1. Gentry, R. V., Science, 184, 62 (1974).
2. Kohnan, T. P., Ann. N. Y. Acad Sci., 62, 503 (1956).
3. Henderson, G. H., Mushkat, C. M., and Crawford, D. P., Proc. R. Soc., A158, 199 (1934); Henderson, G. H., and Turnbull, L. G., ibid., 145, 582 (1934); Henderson, G. H., and Bateson, S., ibid., 573 (1934).
4. Gentry, R. V., Ann. Rev. NucI. Sci., 23, 347 (1973).
5. Gentry, R. V., Cristy, S. S., McLaughlin, J. F., and McHugh, J. A., Nature, 244, 282 (1973).
6. Gentry, R. V., Science, 173, 727 (1971).

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