We have detected a concentration of boron in martian clay far in excess of that in any previously reported extra-terrestrial object. This enrichment indicates that the chemistry necessary for the formation of ribose, a key component of RNA, could have existed on Mars since the formation of early clay deposits, contemporary to the emergence of life on Earth. Given the greater similarity of Earth and Mars early in their geological history, and the extensive disruption of Earth's earliest mineralogy by plate tectonics, we suggest that the conditions for prebiotic ribose synthesis may be better understood by further Mars exploration.
Citation: Stephenson JD, Hallis LJ, Nagashima K, Freeland SJ (2013) Boron Enrichment in Martian Clay. PLoS ONE 8(6): e64624. https://doi.org/10.1371/journal.pone.0064624
Editor: Stefan Maas, NIGMS, NIH, United States of America
Received: March 12, 2013; Accepted: April 16, 2013; Published: June 6, 2013
Copyright: © 2013 Stephenson et al. This is an open-access article distributed under the terms of the Creative Commons Attribution License, which permits unrestricted use, distribution, and reproduction in any medium, provided the original author and source are credited.
Funding: This material is based upon work supported by the National Aeronautics and Space Administration through the NASA Astrobiology Institute under Cooperative Agreement No. NNA09DA77A issued through the Office of Space Science. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript.
Competing interests: The authors have declared that no competing interests exist.
The sugar ribose is central to metabolism, most notably as the derivatized sugar component of RNA. Any theory of life’s origins focused on RNA must therefore include a plausible prebiotic ribose production pathway , . Borate minerals have been shown to stabilize ribose ,  synthesized via the formose reaction , making boron a potentially important chemical element connecting geoscience to organic chemistry. One of the main objections to this mode of ribose accumulation on the early Earth is that evaporitic borate deposits (e.g. colemanite, ulexite and kernite) may not have been present on the early Earth (>3.5 Ga) . Our research suggests boron-enriched clay as an alternative site for ribose production.
Clays have long been proposed as excellent locations for prebiotic catalysis , , polymerization , , and compartmentalization  because of their ability to absorb and protect necessary reactants . These properties are evident in the popularity of clays as catalysts within industry . Boron is commonly concentrated as borate (BO33− or BO43−) in terrestrial clays and organic-rich sediments (∼80–800 ppm), but it has never been found at concentrations above 20ppm in any extraterrestrial source (Figure 1, Table S1). Here we use secondary ion mass spectrometry to show that Earth-like boron concentrations exist in martian clay.
Comparison data was from chondrite meteorite phases, martian meteorite primary and alteration phases (including clays), terrestrial clays and coals. Measured data from the Sutter’s Mill chondrite and from martian meteorite MIL 090030 show similar or reduced boron concentrations to their previously measured equivalents. The degree of boron enrichment in MIL 090030 clay data is most closely comparable to terrestrial clays, it is highly enriched compared to other phases in the same meteorite and to previously measured martian clays. Error bars are 2σ.
Results and Discussion
Martian meteorite MIL 090030 was collected in the Miller Range region of Antarctica during the 2009/10 ANSMET field season. It belongs to the nakhlite group of martian meteorites - basaltic lavas that crystallized ∼1.3 billion years ago , . Subsequent to crystallization these meteorites were aqueously altered on Mars, which produced narrow (generally <100 µm wide) alteration veins containing evaporite salts, amorphous silicate, Fe-oxides and smectite clays –. We determined the abundance of boron in the alteration veins of MIL 090030, via in-situ Cameca ims 1280 ion-microprobe analyses at the University of Hawaii (Materials and Methods). For comparison we also analyzed the primary igneous minerals of MIL 090030, as well as various primary and aqueous alteration phases in Sutters Mill – a carbonaceous chondrite meteorite observed to fall in 2012 .
The abundances of boron measured in Sutter’s Mill olivine and matrix material (Table 1) are comparable to data previously reported for boron in the carbonaceous chondrites (0.004–0.7 ppm) . Furthermore, boron abundances in the igneous primary minerals (olivine and pyroxene) of MIL 090030 are comparable to those of the carbonaceous chondrites (Table 1). In contrast, boron is concentrated in martian alteration veins (∼160 ppm), to levels rivaling those found in terrestrial clays and marine sediments (Figure 1). The level of boron concentration in the alteration veins of MIL 090030 cannot be explained by terrestrial contamination, as no atmospheric reservoir on Earth approaches the abundance of boron measured in these alteration veins (Figure 1). However, as smectite clays and amorphous materials can readily adsorb atmospheric and aqueous contaminants, both an exterior (MIL090030,25) and interior (MIL 090030,23) sample from the MIL 090030 meteorite stone were measured. We found no measureable difference between boron abundances in the alteration veins of the internal and external areas, implying terrestrial boron is negligible. In addition, heavy pre-sputtering prior to each ion-probe analysis (Figure S1 and Figure S2) removes any surface contamination which may result from sample preparation (Materials and Methods). Therefore, the boron concentration in MIL 090030 alteration veins must be the result of secondary alteration processes on Mars.
Boron is readily adsorbed onto clay surfaces , , and has a greater affinity for smectite and illite than for other clay species –. Given that MIL 090030 alteration veins contain smectite it follows that boron enrichments should be found in these veins. However, the degree of enrichment reported here is somewhat surprising - an order of magnitude higher than any other extraterrestrial phase investigated to date , , .
A straightforward geochemical interpretation of our results is that boron, a relatively volatile and soluble element, was first concentrated in the fluid dregs of lava (4–7 ppm boron has been detected in the late stage mesostasis of other nakhlites ) and then became further concentrated by any groundwater or hydrothermal fluids that came into contact with the rock. Due to the oxidizing conditions of martian clay the boron most likely exists as borate, possibly in isolation or else bound to cations such as calcium, magnesium or sodium.
Borates may be crucial to prebiotic chemistry due to their ability to stabilize ribose, a key component of RNA. Without them, ribose degrades, reducing it to only a small fraction of the formose reaction products –. With borate ribose can last months. This results in a relative enrichment of ribose and other aldopentoses  compared to other formose products , . Clays have long been implicated as ideal catalytic surfaces for prebiotic reactions , hence borate enriched martian clay may represent a potential site for ribose synthesis.
MIL090030 offers a glimpse into the chemistry of Mars at the time of its clay’s formation, but coupled with other data it also offers some insight into the potential of earlier clays. Remote sensing observations of the martian surface ,  suggest an early (>3.7 Ga) wet environment, compared to the later, relatively dry conditions under which the MIL 090030 clays formed. During this earlier and wetter clay-forming period Fe-smectite clays similar to those found in MIL 090030 were dominant . Hence, there is no reason to assume the earlier clays were comparatively boron depleted. Gale crater, which is currently being explored by the Curiosity rover, contains Fe-smectite units within its layered deposits , which may have formed in a lake environment on early Mars (3.6–3.8 Ga) .
This old (>3.7 Ga), relatively wet period in Mars history is contemporaneous with current estimates for the origin of life on Earth. Similar clay deposits to those produced in this wet martian environment appear to have formed on the early Earth as well. For example, intensively studied ancient (3.8 Ga) tourmaline grains from western Greenland appear to have formed from boron-rich clay precursors , . Given the greater similarity of Earth and Mars early in their geological history, further exploration of Mars may prove invaluable in answering how ribsose may have accumulated on the Earth prebiotically.
Materials and Methods
Sample Preparation and Petrographic Analysis
We were allocated two thin-sections of the nakhlite martian meteorite MIL 090030 by CAPTEM, prepared in 2011 at the NASA Johnson Space Center. MIL 090030,25 was deliberately cut from the external surface of the ∼450 g parent meteorite, whereas MIL 090030,23 was taken from the central portion. One thin-section (#51) of the Sutter’s Mill meteorite, which was seen to fall in California in 2012, was allocated to UH by Q.-Z. Yin at UC Davis. This section of Sutter’s Mill has been identified as a CM2.0/CM2.1-type carbonaceous chondrite .
We utilized the JEOL JSM-5900LV scanning electron microscope at the University of Hawaii (UH) to produce whole-thin-section backscatter-electron images and elemental X-ray images at low resolution (20 µm pixel size), in order to locate areas of interest. These areas were subsequently X-ray imaged at higher resolutions, with various pixel sizes (1–5 µm), to determine the best places for ion microprobe analyses. To verify the positions of the sputtered regions, these areas were also imaged after analyses.
The major- and minor-element chemistry of each phase was determined via JEOL JXA-8500F electron microprobe (EMP) analyses at UH (Table S2). The analytical conditions of the electron microprobe included a 10 nA primary beam current, 15 keV accelerating voltage, and 5 µm spot size. The count time for beam-sensitive elements (e.g., Na and K) was set at 15 s, whereas that for less sensitive elements was set at 30 s. Beam-sensitive elements were measured first. Matrix effects were corrected using PAP procedures. The elemental detection limits are 0.03 wt.% for SiO2, Al2O3, and MgO; 0.04 wt.% for TiO2, CaO, and K2O; 0.06 wt.% for Na2O and Cr2O3; 0.07 wt.% for MnO; 0.08 wt.% for FeO. San Carlos olivine (NMNH 111312) and Rockport fayalite (USNM 85276) were utilized as standards, along with NMNH 117075 chromite. UH standardized orthoclase Or-1 (5–168), Lake County labradorite, Kakanui augite, Amelia Albite, Sphene glass and Verma garnet were also used as standards.
All three of these thin-sections were prepared using epoxy resin. EMP analyses suggest this resin contains trace amounts of boron (<0.01 wt %). Therefore, all areas close to epoxy were carefully avoided as potential sites for boron abundance analysis. None of our analysis areas contain epoxy within the pre-sputtered region, as evidenced by X-ray imaging.
Boron Abundance Analyses
The ions of boron (11B+), calcium (40Ca+) and magnesium (26Mg+) in both standard materials and unknowns were measured in situ using the UH Cameca ims 1280 ion microprobe, with a primary 16O− ion beam accelerated to 13 keV and an impact energy of 23 keV. Positively charged secondary ions were accelerated to +10 keV and an energy window of 50 eV was used. 40Ca and 26Mg were measured to provide internal standardization for calcium and magnesium rich phases, respectively (Equation 1 and Equation 2) – the true wt % values of these elements for each analysis area were measured via electron microprobe analysis, as discussed above. To minimize possible surface contamination of boron, a 10nA focused 16O− primary ion beam was rastered over 30×30 µm area for 1000 seconds. The data were collected with a 1nA focused primary beam rastered over 10×10 µm area at the center of the pre-sputtered area (Figure S1, Figure S2). The count rates of 11B+ during measurements did not show systematic decrease with time and were typically constant within their errors, indicating that the pre-sputtering procedure completely removed any surface contamination. The mass resolving power was ∼2000, sufficient to separate any interfering molecules. 11B+ was measured on an electron multiplier while 26Mg+ and 40Ca+ were measured by a Faraday cup. Each measurement consisted of 30 cycles, with 11B measured for 20s, 26Mg for 2s, and 40Ca for 2s during each cycle. The background count rate of the electron multiplier is ∼0.002 cps. Under these conditions, the detection limit of B was less than 1 ppb .
Data were corrected for sensitivities among B, Ca, and Mg using USGS basaltic glass standards BCR-2G and GSA-1G, containing 6±1 ppm and 23±7 ppm boron, respectively (from GeoRem data base, ). BCR-2G was prepared by melting kilogram aliquots of (powdered) BCR-2 (Columbia River basalt), BHVO-2 (Hawaiian Volcanic Observatory basalt), and BIR-1 (Icelandic basalt), at 1540°C under a nitrogen atmosphere. GSA-1G was prepared using a set of synthetic glass powders - it has an overall basaltic composition but is doped with more than fifty trace elements at concentrations of <0.1 µg g−1. Repeat analyses of these standards allow for the calculation of sensitivity factor (Equation 1). Both 26Mg and 40Ca are abundant in the glass standards, and so either could be used to calculate sensitivity factor, in Equation 1 26Mg is used as an example:(1)
The sensitivity factor, in turn, allows for the calculation of the concentration of B in the unknown Equation 2. Again, depending on the composition of the unknown, either 26Mg or 40Ca was used. We used 26Mg for most phases as it was most abundant in olivine, pyroxene, the martian alteration veins (containing the smectite clay), and the matrix of Sutter’s Mill. However, we did use 40Ca for calcite and dolomite.(2)
The sensitivity factors obtained for the two basaltic glass standards have a systematic difference of ∼40–50% (Table S3). The reported errors include this uncertainty.
Our boron analysis methodology is similar to that reported by  who used glass standards to determine boron abundance in smectite clays. These authors reported matrix effects to be unnoticeable. As discussed in detail by , matrix affects between glasses and crystalline phases are small (<10%) when Si is used for normalization. If Mg or Ca are used instead of silicon (as in this study), these affects are reduced further.
Secondary electron images of Cameca ims 1280 ion microprobe analysis pits in Sutters Mill. The extent of the 30 µm pre-sputtering raster is clearly visible as a slightly lighter grey area around the central 10 µm analysis pit of olivine (olv) 1 (A). Due to their smaller grain size, the pre-sputtering raster goes beyond the boundaries of calcites 1 and 2, and dolomite 1, but the central pit is within these carbonates (B–D). The heterogeneous nature of the matrix in Sutter’s Mill makes it more difficult to distinguish the extent of the analysis pits (E–H). However, our data suggest that despite this heterogeneity the matrix is relatively uniform with respect to boron.
Secondary electron images of Cameca ims 1280 ion microprobe analysis pits in MIL 090030,23 (A–F) and MIL 090030,25 (G–H). As in Figure S1, the pre-sputtered 30 µm region in these images is visible as a slightly lighter grey area surrounding the central 10 µm analysis pit (labels mark the extent of this area). For alteration vein analyses the pre-sputtered area extends beyond the margins of the vein. However, all central analysis pits lie within these margins. MIL 090030,25 alteration vein 1 exhibits weathered olivine around its margins. All visible cracks are empty of epoxy resin (as evidenced by X-ray imaging). Olv = olivine, cpx = clinopyroxene.
Previously published boron reservoir data.
Representative major and minor element abundances.
Glass standard measured boron abundances.
Sutters Mill sample #51 was allocated to the University of Hawaii by Q.-Z. Yin at UC Davis. Eric Hellebrand is thanked for his help with electron microprobe X-ray imaging.
Conceived and designed the experiments: JDS SJF. Performed the experiments: LJH JDS KN. Analyzed the data: LJH KN. Contributed reagents/materials/analysis tools: KN. Wrote the paper: JDS LJH SJF.
- 1. Szostak JW (2012) The eightfold path to non-enzymatic RNA replication. J Syst Chem 3: 2.
- 2. Deamer D, Weber AL (2010) Bioenergetics and Life's Origins. Cold Spring Harb Perspect Biol 2: a004929.
- 3. Ricardo A, Carrigan MA, Olcott AN, Benner SA (2004) Borate minerals stabilize ribose. Science 303: 196.
- 4. Kim HJ, Benner SA (2010) Comment on “The silicate-mediated formose reaction: bottom-up synthesis of sugar silicates”. Science 20(329): 5994.
- 5. Boutlerow MA (1861) Formation synthétique d'une substance sucrée. Comptes Rendus des Seances de l’a Academie des Sciences 53: 145–147.
- 6. Grew ES, Bada JL, Hazen RM (2011) Borate minerals and the origin of the RNA world. Orig Life Evol Biosph 41: 307–316.
- 7. Cairns-Smith AG (1985) Seven Clues to the Origin of Life: A Scientific Detective Story: Cambridge University Press.
- 8. Fripiat JJ, Cruz-Cumplido MI (1974) Clays as Catalysts for Natural Processes. Annual Review of Earth and Planetary Sciences 2: 239–256.
- 9. Ferris JP, Hill AR Jr, Liu R, Orgel LE (1996) Synthesis of long prebiotic oligomers on mineral surfaces. Nature 381: 59–61.
- 10. Joshi PC, Aldersley MF, Delano JW, Ferris JP (2009) Mechanism of Montmorillonite Catalysis in the Formation of RNA Oligomers. J Am Chem Soc 131: 13369–13374.
- 11. Hanczyc MM, Fujikawa SM, Szostak JW (2003) Experimental Models of Primitive Cellular Compartments: Encapsulation, Growth, and Division. Science 302: 618–621.
- 12. Pucci A, Branciamore S, Casarosa MD, Acqui LP, Gallori E (2010) Implications For An RNA-Clay World: Interaction Of Cytosine With Clay Minerals. J Cosmology 10: 3398–3407.
- 13. Chitnis SR, Sharma MM (1997) Industrial applications of acid-treated clays as catalysts. React Funct Polym 32: 93–l15.
- 14. Stauffer H (1962) On the production rates of rare gas isotopes in stone meteorites. J. Geophys. Res 67: 2023–2028.
- 15. Okazaki R, Nagao K, Imae N, Kojima H (2003) Noble gas signatures of Antarctic nakhlites, Yamato (Y-000593, Y-000749, and Y-000802. Antarct Meteor Res 16: 58–79.
- 16. Gooding JL, Wentworth SJ, Zolensky E (1991) Aqueous alteration of the Nakhla meteorite. Meteoritics 26: 135–143.
- 17. Treiman AH, Barrett RA, Gooding JL (1993) Preterrestrial aqueous alteration of the Lafayette (SNC) meteorite. Meteoritics 28: 86–97.
- 18. Changela HG, Bridges JC (2011) Alteration assemblages in the nakhlites: Variation with depth on Mars. Meteorit Planet Sci 45: 1847–1867.
- 19. Hallis LJ, Taylor GJ (2011) Comparisons of the four Miller Range Nakhlites, MIL 03346, 090030, 090032 and 090136: Textural and compositional observations of primary and secondary mineral assemblages. Meteorit Planet Sci 46: 1787–1803.
- 20. Jenniskens P, Fries MD, Yin Q-Z, Zolensky M, Krot AN, et al. (2012) Radar-Enabled Recovery of the Sutter’s Mill Meteorite, a Carbonaceous Chondrite Regolith Breccia. Science 338: 1583.
- 21. Sugiura N, Shuzou Y, Ulyanov A (2001) Beryllium-boron and aluminium-magnesium chronology of calcium-aluminium-rich inclusions in CV chondrites. Meteorit Planet Sci 36: 1397–1408.
- 22. Schwarcz HP, Agyei EK, McMullen CC (1969) Boron isotopic fractionation during clay adsorption from seawater. Earth Planet Sci Lett 6: 1–6.
- 23. Brumsack HJ, Zulegar E (1992) Boron and boron isotopes in pore watersfrom ODP leg 127, sea of Japan. Earth Planet Sci 113: 427–433.
- 24. Hingston FJ (1964) Reactions between boron and clays. Aust. J Soil Res 2: 83–95.
- 25. Couch EL, Grimm RE (1968) Boron fixation by illites. Clays and clay minerals 16: 249–256.
- 26. Keren R, Mezuman V (1981) Boron adsorption by clay minerals using a phenomenological equation. Clays and clay mins 29: 198–204.
- 27. Anders E, Grevess N (1989) Abundances of the elements: Meteoritic and solar. Geochim Cosmochim Acta 53: 197–214.
- 28. Spivak-Birndorf LJ, Wadhwa M, Williams LB (2008) Paper presented at Goldschmidt Conference.
- 29. Decker P, Schweer H, Pohlamnn R (1982) Bioids : X. Identification of formose sugars, presumable prebiotic metabolites, using capillary gas chromatography/gas chromatography–mass spectrometry of n-butoxime trifluoroacetates on OV-225. J Chromatogr A 244(2): 281–291.
- 30. Larralde R, Robertson MP, Miller SL (1995) Rates of decomposition of riboseand other sugars: Implications for chemical evolution. Proc Natl Acad Sci U.S.A. 92: 8158–8160.
- 31. Shapiro R (1988) Prebiotic Ribose Synthesis: a critical analysis. Orig Life Evol Biosph 18: 71–85.
- 32. Kim HJ, Ricardo A, Illangkoon HI, Kim MJ, Carrigan MA, et al. (2011) Synthesis of carbohydrates in mineral-guided prebiotic cycles. J Am Chem Soc 133(24): 9457–9468.
- 33. Murchie SL, Mustard JF, Ehlmann BL, Milliken RE, Bishop JL, et al. (2009) A synthesis of martian aqueous mineralogy after 1 Mars year of observations from the Mars Reconnaissance Orbiter. J Geophys Res 114: E00D06.
- 34. Ehlmann BL, Mustard JF, Murchie SL, Bibring J-P, Meunier A, et al. (2011) Subsurface water and clay mineral formation during the early history of Mars. Nature 479: 53–60.
- 35. Wary JJ (2013) Gale crater: the Mars Science Laboratory/Curiosity Rover Landing Site. Int J Astrobio 12: 25–38.
- 36. Thomson BJ, Bridges NT, Milliken R, Baldridge A, Hook SJ, et al. (2011) Constraints on the origin and evolution of the layered mound in Gale Crater, Mars using Mars Reconnaissance Orbiter data. Icarus 214: 413–432.
- 37. Appel PWU (1995) Tourmalines in the 3800 Ma old Isua supracrustal belt, West Greenland. Chem Geol 72: 227–234.
- 38. Chaussidon M, Appel PWU (1997) Boron isotopic composition of tourmalines from the 3.8-Ga-old Isua supracrustals, West Greenland: implications on the 11B value of early Archean seawater. Chem Geol 136: 171–180.
- 39. Wielandt D, Nagashima K, Krot AN, Huss GR, Ivanova MA, et al.. (2012) Evidence for multiple sources of Be in the early solar system. Astrophys J Lett 748: L25,7.
- 40. Jochum KJ, Willbold M, Raczek I, Stoll B, Herwig K (2005) Chemical Characterisation of the USGS Reference Glasses GSA-1G, GSC-1G, GSD-1G, GSE-1G, BCR-2G, BHVO-2G and BIR-1G Using EPMA, ID-TIMS, ID-ICP-MS and LA-ICP-MS. Geostand Geoanal Res 29: 285–302.
- 41. Williams LB, Hervig RL, Hutcheon I (2001) Boron isotope geochemistry during diagenesis. Part II. Applications to organic-rich sediments. Geochim Cosmochim Acta 65(11): 1783–1794.
- 42. Hervig RL (1996) Analyses of geological materials for boron by secondary ion mass spectrometry. In, Boron: Mineralogy, petrology and geochemistry Rev Mineral 33: 789–803.