We determined concentration profiles of Ne-21, Ne-22, and Ar-38 produced by solar protons as a function of depth in oriented lunar rock 68815. A comparison with model predictions indicate a solar proton flux J(4(pi)(r); E greater than 10 MeV) of 100-125 p/sq. cm/s and a rigidity, R sub 0, of 85-100 MV, assuming an erosion rate of 1-2 mm/Myr. These results for 68815 and similar results on 61016 define the integrated solar proton energy spectrum at the moon over the past approximately 2 Myr

Bogard, D. D.

Garrison, D. H.

Rao, M. N.

English

NASA Technical Reports Server

/. LPSC XXIV 521
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SCR 21Ne AND 38At IN LUNAR ROCK 68815: THE SOLAR PROTON ENERGY
SPECTRUM OVER THE PAST 2 MYR; D. H. Garrison 1, M. N. Rao 2, D. D. Bogard
(NASA Johnson Space Center, Houston, TX 77058; 1-also Lockheed-ESC; 2-also Lunar & Planetary Inst.),
and R. C. Reedy (Los Alamos Natl. Lab., Los Alamos, NM 87545)
Abstract: We determined concentration profdes of 2tNe, 22Ne, and 38Ar produced by solar protons as a
function of depth in oriented lunar rock 68815. A comparison with model predictions indicate a solar proton
flux J(_; E > 10 MeV) of 100-125 p/cmZ/s and a rigidity Ro of 85-100 MV, assuming an erosion rate of 1-2
mm/Myr. These results for 68815 and similar results on 61016 define the integrated solar proton energy
spectrum at the moon over the past -2 Myr.
Previous Work: For oriented rock 61016, which like 68815 has a simple -2 Myr exposure history [1], we
recently resolved SCR 21Ne, 22Ne, and 38At produced by nuclear interactions of energetic (-10-100 MeV) solar
protons [2,3]. Concentrations of the SCR component significantly decreased with sample depth and gave the
first depth profdes for stable, SCR nuclides. The 2tNe/22Ne ratios produced by solar (SCR) and galactic
(GCR) protons were easily resolved. These SCR concentration profdes matched theoretical production profiles
for a 4fr proton flux above 10 MeV of J = 100 p/cm2/s and an exponential rigidity spectral parameter [4,5], Ro,
between 70 and 85 MV [3]. Several investigators have reported in 68815 the presence of SCR radionuclides
[6,7,8,9] and possibly of SCR 3He and ZiNc [10]. The 26A1 and 53Mn depth profiles were consistent with J> 10
=70 p/cm2/s and Ro = 100 MV [6]; the profile for SCR 14C (in the same 68815,292 depth column as our
samples) yielded J > 10 = 144 p/cmZ/s at Ro = 85 MV, or J > 10 = 91 p/cmZ/s at Ro = 100 MV [7]; depth profiles
of SCR 81Kr suggested J > 10 = 160 p/cm2/s at Ro = 85 MV [8]. The nearly flat depth profde for 1°Be in 68815
suggested a softer proton spectral shape than previous work [9].
Expetimentak From 10 carefully prepared and documented depth samples (0 to 4.3 cm) of 68815,292,
gases were extracted in either two or three temperature steps of .500°C and 1600°C or 350°C, 950°C, and
1600°C. Isotopic abundances were determined by mass spectrometer, using techniques previously described [3].
Chemical composition of the samples (electron microprobe analysis by V. Yang, NASA/JSC) indicated a
mixture of 80% plagioclase, 12% olivine/pyroxene, and 8% glass. The Mg concentration is 3.74%.
68815 Results: A 3-isotope correlation plot for all neon data (Fig. 1) indicate mixing between an implanted
solar component with 2°Ne/22Ne = 12.6 (determined by the surface sample) and a cosmogenic component with
variable composition. (All samples released solar-implanted Ne and At, some at 1600°C, which we assume was
incorporated into high temperature glass phases during breccia formation.) The theoretical field shown for
SCR Ne was calculated using the measured major elemental concentrations, and, due to the presence of Mg,
ties slightly closer to GCR Ne in 68815 than in 61016. The isotopic variation of cosmogenic Ne in 68815 is
attributed to variable mixtures of solar proton-produced (SCR) Ne with galactic-produced (GCR) Ne and is
shielding dependent over the range represented by these sample depths. Extrapolation of temperature data for
individual samples to cosmogenic 2°Ne/22Ne = 0.9 suggests a cosmogenic 21Ne/ZZNe end-point for surface
samples of -0.66. This ratio is similar to the SCR + GCR value of 0.64 observed in 61016 and the predicted
value of 0.65 for the composition and shielding of 68815.
Total (GCR + SCR) cosmogenic 21Ne and 3BAr concentrations for each sample are plotted vs. depth in
Figs. 2a and 2b. Cosmogenic 22Ne concentrations show a profde similar to 21Ne. Surface-implanted neon and
argon were removed by lever rule correction assuming trapped 2°Ne/ZZNe = 12.6 and 36Ar/38Ar = 5.35.
Cosmogenic 21Ne and 38At comprise 84.5-99.8% and 23-84.6%, respectively, of the total isotopic releases.
Since GCR production rates vary tittle over 0-43 ram, the systematic increase in concentrations of cosmogenic
21Ne and 3BAr with decreasing shielding is due to production by solar protons. These SCR production profiles
are similar to the 21Ne and 3BAr profdes found in lunar rock 61016 [2,3] and to radionuclide proFdes measured
in 68815 [6-9]. Assuming the ZlNe concentration of 0.184 x 10-8 cm3STP/g in the deepest sample (42 ram)
represents only GCR production, and assuming a production rate of 0.099 xl0 -8 cm3STP/g/Myr [11], we obtain
a GCR exposure age of 1.8 Myr. Similarly, "the cosmogenic 38At concentration of 0.195 xl0 -8 cm3STP/g
measured in the same sample and a production rate of 0.11 xl0 -8 em3STP/g/Myr [11] gives a GCR exposure
age of 2.1 Myr. Considering uncertainties in production rates and absolute abundance, these exposure ages
suggest that < 10% of the 21Ne and 38At concentrations in the 42.8 mm sample are due to SCR production.
Solar Proton Energy Spectrum: We now compare the SCR depth profiles with theoretical predictions for
different proton fluxes, rigidity, and surface erosion rates. Theoretical SCR + GCR production curves [4,5] are
shown (Fig. 2) for a 4rr proton flux J (E > 10 MeV) of 100 p/cm2/s and four values of Ro. Each theoretical
https://ntrs.nasa.gov/search.jsp?R=19940011704 2020-06-16T20:29:53+00:00Z
522 LPSCXXIV
SCRNe& Ar in68815:SOLARPROTONENERGYSPECTRUM;Garrisonetal.
profileisnormalizedto thedeepestample,usesameasuredrockdensityof2.3g/cms, and assumes a surface
erosion rate (Q) of i mm/Myr and a depth-constant GCR component. Profde shapes are not especially
sensitive to Q or sample density, but are more sensitive to J and Ro [3]. Because variations in J and Ro have
opposite effects on the curve fit, only ranges and not unique values can be derived. Additional constraints are
the close agreement between calculated and expected GCR exposure ages and the observation that Ne isotopic
ratios from the deeper samples fall close to expected GCR values (Fig .1). Both observations indicate < 10%
SCR production at depths of -42 mm, and thus provide an upper limit to Ro of "100 MV. The values of J, Ro,
and Q which give the best fit to the data were determined using a least squares technique where all parameters
but one were fixed, the optimal value of the variable determined by iteration, and the process repeated for
different ftxed parameter values. This yielded optimal fit combinations for J = 90-140 p/cm2/s and Ro = 85-
100 MV. For a depth-variable GCR component, the optimal range of values of Ro stays the same, but the
values of J and the SCR component at 42 mm depth increase somewhat, the latter usually exceeding our 10%
limit. No values of Ro as low as 70 MV gave optimal fits to the data. Values of Q = 0-3 mm/Myr are all
possible within these optimal fits; higher values of Q give higher values of J.
Oriented lunar rocks 68815 and 61016 provide our best evidence for the long-term flux and energy
spectrum of solar protons. From Ne and Ar results, we conclude that the best parameters to describe the
average solar energy spectrum over the past 2 Myr are J= 100-125 p/cm2/s, Ro=85-100 MV, and erosion = 1-2
mm/Myr. These ranges can be further constrained by fudng specific parameters. The 68815 and 61016 Ne and
Ar profdes imply a solar proton spectrum that is less energetic than that suggested by earlier radionuelide data
[6], but similar to more recent radionuclide data [7-9].
References: [1] Walker and Yuhas Proc. LPSC 4, 2379-23879 (1973); [2] Rap et al., LPSCXXII (alas), 1111
(1991); [3] Rap et al., Z Geophys. Res., Sp. Phys.(in press); [4] Reedy and Arnold, J. Geophys. Res. 77, 537-555
(1972); [51 Reedy, LPSCXXIII (abs), 1133 (1992); [6] Kohl et al., Proc. LPSC 9, 2299-2310 (1978); [7] jull et al.,
LPSC 23 (abs), 630-640 (1992); [81 Reedy & Marti, The Sun in Time, 260-287 (1991); [9] Nishiizumi et al., Proc.
LPSC 18, 79-85 (1988); [10] Yaniv and Marti, Astrophys. J. Lett. 247, L143-146 (1981); [11] Hohenberg et al.,
Proc. LPSC 9, 2311-2344 (1978).
Fig. 1 (Below) Neon 3-isotope correlation plot for temperat_e extractions of depth samples of 68815.
Uncertainties are -1% and fall within the symbols. The 350uC data (not shown) represent 0.4-2% of the total
release (except 0.1 mm sample). Implanted solar wind and solar flare compositions and the theoretical SCR Ne
field produced in situ by energetic solar protons are also shown.
Fig. 2 (Right) Cosmogenic 21Ne (upper) and 3BAr (lower) concen- 3.2
trations (symbols) vs. depth from the rock surface. Uncertainties
are -+ 3%, or approximately twice the symbol size. Sample thick- ._ 3.0
hess ranged from -lmm near the surface to -3ram at the deepestlocation. Surface samples with > 96% solar-implanted Ne and Ar 2.8
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are not shown. Lines represent theoretical SCR concentrations o 2.6
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The SCR Ne-21 and Ar-38 in lunar rock 68815: The solar proton energy spectrum over the past 2 MYR

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