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Taking the pulse of Mars via dating of a plume-fed volcano

  • Nature Communications 8, Article number: 640 (2017)
  • doi:10.1038/s41467-017-00513-8
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Abstract

Mars hosts the solar system’s largest volcanoes. Although their size and impact crater density indicate continued activity over billions of years, their formation rates are poorly understood. Here we quantify the growth rate of a Martian volcano by 40Ar/39Ar and cosmogenic exposure dating of six nakhlites, meteorites that were ejected from Mars by a single impact event at 10.7 ± 0.8 Ma (2σ). We find that the nakhlites sample a layered volcanic sequence with at least four discrete eruptive events spanning 93 ± 12 Ma (1416 ± 7 Ma to 1322 ± 10 Ma (2σ)). A non-radiogenic trapped 40Ar/36Ar value of 1511 ± 74 (2σ) provides a precise and robust constraint for the mid-Amazonian Martian atmosphere. Our data show that the nakhlite-source volcano grew at a rate of ca. 0.4–0.7 m Ma−1—three orders of magnitude slower than comparable volcanoes on Earth, and necessitating that Mars was far more volcanically active earlier in its history.

Introduction

On Earth, the majority of volcanism and planetary heat loss occurs by plate tectonics, a process driven by mantle convection1, with most volcanoes being active along divergent and convergent plate boundaries. A small proportion of terrestrial volcanoes are fed by mantle plumes—highly localized upwellings of abnormally hot rock that ascend from deep within the mantle and undergo partial melting at relatively shallow depths2. Mars, on the other hand, has lacked plate tectonics for most of its history3, 4. The static ‘stagnant lid’ of the thick Martian lithosphere has restricted convective heat loss1, leaving mantle plumes as the dominant, but less efficient, mechanism for transferring heat from the planet’s core to its surface3, 5. Tectonic activity continually moves the Earth’s lithospheric plates over mantle plumes, forming age-progressive chains of volcanoes2. Even in cases of the slowest-moving plates, individual plume-derived volcanoes on Earth are only active for a few million years6. Conversely, Martian plume-fed edifices have remained connected to their magma sources for extraordinary lengths of time—in some cases for billions of years5, 7, 8. As a consequence, although morphologically similar to shield volcanoes on Earth, Martian volcanoes have grown to be the largest in the solar system9 (Fig. 1).

Fig. 1
Fig. 1

Distribution and size of Martian volcanoes. a Amazonian volcanic products on Mars (digital elevation model and orange outlines 43) are located in the Tharsis and Elysium regions, with the largest volcano, the 600 km wide Olympus Mons, rising more than 21 km above the surrounding plains. The red star in the Elysium region marks the location of a potential source crater for the nakhlites42. b Relative characteristics of terrestrial and Martian plume volcanism. In comparison to terrestrial volcanoes (blue) those on Mars (red) have a greater volume and duration, but much lower eruption rates. Data and references in Supplementary Table 1

Radioisotopic dating has been used to determine the lifespans (typically <2 Ma) and eruption rates (typically >1000 m Ma−1 and 10,000 km3 Ma−1) of individual plume volcanoes on Earth10 (Fig. 1b), but such approaches have not been applied to Mars. Crater-counting model ages11, an approach to estimating the age of a planetary surface based upon the size-frequency distribution of impact craters, indicate that Martian volcanoes have longer lifespans (up to 3500 Ma) but far lower eruption rates (<10 m Ma−1 and <700 km3 Ma−1) (Fig. 1b and Supplementary Table 1). These crater-counting models are useful to resolve the relative ages of planetary surfaces, but are prone to uncertainty in terms of absolute age determination. This is because the crater counting technique makes several assumptions, including the assessment of the differing impactor flux between Mars and the Moon, the extent of crater burial (e.g., by Martian regolith) and the classification of primary vs secondary craters11, 12. By instead targeting a unique set of meteorites, the nakhlites, we have sought to accurately determine the age and growth rate of a volcanic system on Mars using high-precision 40Ar/39Ar dating.

The nakhlites comprise 18 meteorites (not accounting for pairing). Their bulk chemistry is basaltic, with abundant clinopyroxene, less common olivine and a rapidly quenched fine-grained mesostasis comprising feldspar and accessory phases, including chlorapatite and volcanic glass13. The nakhlites are also notable for the presence of phyllosilicates and carbonates—products of low-temperature water-rock interaction on Mars13. These rocks are mineralogically, chemically and isotopically similar—but not identical13,14,15. Their cosmogenic exposure ages cluster around 11 Ma, indicating the different meteorites spent a similar duration in space while transiting from Mars to the Earth15, 16. These data have been employed to suggest the nakhlites were excavated from a localized region of a Martian volcano by a single impact event13, 16. During impact and spallation, the nakhlites experienced mild shock metamorphism of 5–20 GPa and ~5–40 °C above ambient17. Despite these low degrees of shock heating17 and their near-pristine mineralogy13, replicate geochronological analyses of the same meteorite disagree; many ages are imprecise and/or fail the robust criteria that define statistical significance (Supplementary Table 2). As such, the temporal relationships between the different nakhlites remain unclear.

In this study, high-resolution (n = 43 to 45 steps) laser step-heating 40Ar/39Ar dating of multiple aliquots (n = 2 to 5) of six nakhlites is applied in conjunction with cosmogenic (38Ar) exposure dating. The cosmogenic exposure dating allows for accurate correction of cosmogenic and chlorine-derived contributions to the bulk isotope measurements and for determination of accurate 40Ar/39Ar age data. The six meteorites analysed span the full range of mineralogical variation observed in the nakhlite group18. The data show that the nakhlites were not all formed during a single cooling event, but instead reveal a protracted volcanic eruption history on Mars.

Results

Argon reservoirs and cosmogenic exposure age

The isotope budgets of meteorites are derived from multiple sources. Martian meteorites contain trapped 40Ar, 38Ar and 36Ar derived from the Martian atmosphere and/or mantle. All meteorites contain variable amounts of cosmogenic 38Ar and 36Ar, which are produced when high-energy cosmic rays interact with atomic nuclei, primarily during the meteorite's journey from Mars to Earth16. Meteorites also contain radiogenic 40Ar (40Ar*), which is ingrown from the radioactive decay of 40K to 40Ar, and accumulates once the rocks have cooled below the closure temperature for 40Ar diffusion. To calculate accurate 40Ar/39Ar ages (a measure of the decay of 40K to 40Ar) it is necessary to establish the contribution of each argon component to the bulk isotope budget of each meteorite19.

Contributions from cosmogenic argon have traditionally been determined using simplifying assumptions regarding the distribution of cosmogenic nuclides and the abundances of 38Ar and 36Ar produced from chlorine during neutron irradiation, which can lead to inaccurate correction of age data19,20,21. The chlorine-derived isotopes are a particular issue for the nakhlite group of Martian meteorites, which can contain over 1000 ppm Cl hosted in salts and/or chlorine-bearing apatite that can be found in the meteorite's mesostasis (Fig. 2 and Supplementary Fig. 1)22. Our preferred method determines the cosmogenic argon correction using a combination of the meteorite’s cosmogenic exposure age determined independently from an un-irradiated fragment, and the step-wise 38Ar and 36Ar cosmogenic production rates calculated from the Ca/K values measured on each 40Ar/39Ar measurement21.

Fig. 2
Fig. 2

Petrology of nakhlite meteorites. Panels ad are scanning-electron microscope images of Nakhla; eh are from Lafayette, and il show a representative area of NWA 5790. Images from the other meteorites (MIL 03346, Yamato 000593 and Yamato 000749) are in Supplementary Fig. 1. Panels a, e, i display the distribution of aluminium (brown), iron (green) and magnesium (blue); panels b, f, j show potassium (red); panels c, g, k illustrate the distribution of phosphorus (blue, concentrated in apatite) and sulphur (magenta, in iron sulphide), as well as the backscattered electron intensity in grey; and panels d, h, l show the distribution of chlorine (green, in apatite). These images illustrate that the nakhlite meteorites are igneous rocks, dominated by euhedral augite crystals set in a fine-grained mesostasis. The augite crystals (deep blue, in a, e, i) are often zoned, with an outer rim of ferroan pigeonite. Olivine crystals are also present, but less common. Potassium is concentrated in mesostasis feldspar. The mesostasis also contains crystals of titanomagnetite (Tmag), iron sulphide (Fe,S) and chlorine-bearing apatite. As potassium and chlorine are both dominantly hosted in the mesostasis, the argon gas derived from radiogenic decay of potassium and chlorine gas from apatite will be closely associated in location and thermal behaviour during a 40Ar/39Ar experiment, and the contribution from chlorine must therefore be accounted for during the cosmogenic argon correction procedure21

We analysed unirradiated fragments of each of the six nakhlites, with our data yielding concordant cosmogenic exposure ages, and a weighted mean of 10.7 ± 0.8 Ma (2σ, 10% uncertainty on production rates; Fig. 3 and Supplementary Table 3). The indistinguishable cosmogenic exposure ages attest to the fact that the nakhlites can be launch-paired, indicating they were ejected from a single point source on the Martian surface by a single impact event. These cosmogenic exposure ages (Fig. 3 and Supplementary Table 3) were used to correct the 40Ar/39Ar data as discussed above21.

Fig. 3
Fig. 3

Cosmogenic exposure dates for the nakhlites. 38Ar cosmogenic exposure ages overlap within uncertainty, which is consistent with all of the nakhlites being sourced from the same impact. Blue data points were analysed at Lawrence Livermore, and red data points were analysed at SUERC. The weighted mean cosmogenic exposure age is 10.7 ± 0.8 Ma (2σ, full external uncertainty, bold text and grey shaded area), which represents the timing of the nakhlite impact event on Mars

Martian atmospheric 40Ar/36Ar composition

An appropriate correction factor for the Amazonian Martian atmosphere was determined via isochron analysis of the 40Ar/39Ar results. Negligible Marian trapped argon components for most of the nakhlites resulted in little variation in 36Ar/40Ar (Supplementary Data 1). However, higher yields of trapped argon in aliquots of Lafayette and Yamato 000593 facilitated isochron regression and calculation of accurate values for the 40Ar/36Ar trapped component. Lafayette yields a trapped 40Ar/36Ar ratio of 1520 ± 400 (2σ) and Yamato 000593 defines a trapped 40Ar/36Ar ratio of 1560 ± 110 (2σ; Fig. 4). These two ratios are indistinguishable, and the latter was used to correct each sample for Martian atmospheric contribution.

Fig. 4
Fig. 4

Trapped Martian 40Ar/36Ar at the time of nakhlite formation. Isochron analysis of a Lafayette and b Yamato 000593 reveal the composition of initial trapped 40Ar/36Ar component. All symbols and results are reported at the two-sigma level. Blue ellipses denote plateau steps that were included in the isochron regression, white ellipses are outliers from the low-temperature steps that were excluded from the isochron analysis, and the red lines indicate the 2σ uncertainty envelope

Nakhlite 40Ar/39Ar geochronology

After the above contributions from cosmogenic and atmospheric argon were accounted for, the 40Ar/39Ar data were plotted on age spectra (Fig. 5 and Supplementary Fig. 2). Plateau ages were defined as contiguous steps that overlap within two-sigma uncertainty, comprising >70% of the 39Ar released23, 24. Twelve of 19 aliquots met this criteria—with many plateaus including >90% 39Ar (Fig. 5 and Supplementary Fig. 2), indicating that the Ar-systematics have been relatively undisturbed. Three aliquots (Lafayette aliquot 02, MIL 03346 aliquot 2 and Yamato 000593 aliquot 3) yielded plateau segments containing between 52 and 59% 39Ar, less than the 70% 39Ar cutoff for plateau ages (Supplementary Fig. 2). Nevertheless, as these three aliquots have plateau segments that are concordant with other aliquots from the same samples that yielded plateaus with >80% of the 39Ar released, we are confident that these three aliquots also record eruption ages. NWA 5790 spectra are more disturbed than the other nakhlites (Fig. 5 and Supplementary Fig. 2). Two of the three aliquots, however, yielded 11 and 13 contiguous steps (ca. 34% 39Ar) that overlap within two-sigma analytical uncertainty. As 24 separate analyses from two different aliquots overlap within analytical uncertainty, we conservatively interpret these data to represent a minimum eruption age for NWA 5790.

Fig. 5
Fig. 5

Representative 40Ar/39Ar age spectra for the nakhlites. Samples are arranged in chronologic order from youngest to oldest: a Lafayette aliquot 01, b Yamato 000593 aliquot 02, c NWA 5790 aliquot 02, d Nakhla aliquot 01, e Miller Range 03346 aliquot 03 and f Yamato 000749 aliquot 01. The top panel of each sample represents the portion of radiogenic Ar (40Ar*) released from each degassing step; the middle panel represents the K/Ca value for each step; and the lower (main) panel shows the calculated 40Ar/39Ar age for each degassing step. All uncertainties are 2σ. The nakhlites yield excellent results, often with statistically robust plateaus comprising >90% of the 39Ar released. NWA 5790 c is an exception, with concordant steps spanning only 34% of the 39Ar released; these results therefore provide only a minimum age constraint for the eruption of this sample. Additional aliquots from these meteorites (n = 2 to 5) are highly reproducible, with similar degassing spectra and concordant plateau ages (Supplementary Figure 2)

The eruption age for each meteorite was calculated as a weighted-mean of all plateau steps. Analytical uncertainties were calculated as the standard error of the mean, but if the mean square weighted deviates (MSWD or reduced chi-squared statistic) was greater than one, the analytical uncertainty was inflated by multiplying the standard error of the mean by the square-root of the MSWD. All samples analysed in this study (including NWA 5790) have plateau and weighted-mean ages with MSWD of less than two, and probability of fit (“p”) values of greater than 0.05 (95% confidence), indicating the analyses are statistically robust23, 24.

Our robust 40Ar/39Ar data are a product of the high-resolution approach to the step-heating experiments25, and employment of procedures21 to make appropriate corrections for cosmogenic and chlorine-derived 36,38Ar—which is important given the aforementioned abundance of chlorine in the nakhlites (Fig. 2, sometimes >1000 ppm Cl22). The highly reproducible age data are consistent with the near-pristine character of the meteorites and associated low degrees of shock metamorphism17. The experimental design25 also facilitated resolution of the different argon reservoirs in each meteorite (Fig. 2a–c).

Discussion

The trapped components previously measured in the nakhlites MIL 03346 (40Ar/36Ar = 1425 ± 230)26 and Yamato 000593 (40Ar/36Ar = 1502 ± 159)27, as well as Chassigny (40Ar/36Ar = 1452 ± 168)27 are commensurate with our analyses (Fig. 4). All of these meteorites crystallized at ca. 1300–1400 Ma (Fig. 5 and ref. 28), and therefore the common trapped component likely reflects the isotopic composition of the Martian atmosphere at that time. The weighted average of these measurements is 1511 ± 74 (2σ) for the 40Ar/36Ar trapped component—the most precise constraint yet obtained for the mid-Amazonian atmosphere of Mars. This value is more precise than, but within analytical uncertainty of, measurements by the Curiosity rover for the present-day Martian atmosphere (1900 ± 600, 2σ)29. It is, however, distinct from the paleo-atmospheric 40Ar/36Ar recorded by the shergottite meteorites (40Ar/36Ar of 1800 ± 100)30, which yield 40Ar/39Ar cooling ages of ca. 180–600 Ma21. Together, these data therefore suggest that the atmospheric 40Ar/36Ar of Mars has increased significantly (Δ 40Ar/36Ar of 300 ± 130) over the last 1300 Ma. The 40Ar/36Ar value of Earth’s atmosphere has likewise increased over time31, and reflects degassing of radiogenic 40Ar from the interior. In the case of Mars, the change in 40Ar/36Ar also provides constraints on atmospheric loss through time32.

The 40Ar/39Ar ages show the nakhlites were erupted between 1416 ± 7 and 1322 ± 10 Ma (2σ, i.e., mid-Amazonian), a period spanning 93 ± 12 Ma (Table 1 and Fig. 6). Our interpretation is that the nakhlites have sampled a layered volcanic sequence, with the 40Ar/39Ar ages defining stratigraphic position (Fig. 6). Two sets of meteorites (respectively: Nakhla and MIL 03346; NWA 5790 and Yamato 000583) are not temporally resolvable at the 2σ level (Fig. 6); however, geochemical and petrographic differences between them15 suggest they may also sample separate flows. A layered volcanic sequence is consistent with the subtle but significant mineralogical, petrological, geochemical and isotopic differences between nakhlites13,14,15, 33, which we interpret as due to changes in magma composition between related—but temporally distinct—extrusive units from the same volcano (Fig. 6). This scenario is unsurprising if one considers an analogy of a moderate-sized bolide hitting a plume-fed shield volcano on Earth (e.g., Mauna Kea, Hawai’i) and the number of chemically similar yet temporally distinct igneous units that could be ejected.

Table 1: 40Ar/39Ar ages for the nakhlites
Fig. 6
Fig. 6

Stratigraphic model for the nakhlite meteorites. a Summary of 40Ar/39Ar age data. Each meteorite has multiple aliquots with highly reproducible plateau ages (red squares). Bold black squares and horizontal grey bars represent weighted mean ages. The 40Ar/39Ar results indicate that the nakhlites were erupted in at least four temporally discrete eruptions, with volcanic activity spanning 93 ± 12 Ma. All uncertainties are 2σ. b Schematic cross-section for a layered lava flow sequence, with nakhlite stratigraphic relationships and outline of post-impact structure

Our stratigraphic model is consistent with the geology of Martian volcanoes. High-resolution satellite imagery has revealed sequences of lava flows, with individual layers typically 4–26 m thick34, 35, commensurate with the planet’s relatively low gravity that allows for the eruption of numerous thin lava flows that extend for long distances34. Our model of a layered volcanic sequence (Fig. 6) differs from a previous interpretation of the nakhlites that invoked sampling from a single thick flow/intrusive unit18, 36, 37. Such a model where the nakhlites are from a single thick flow or intrusion requires that all of the meteorites would have the same cooling age, which is inconsistent with our 40Ar/39Ar data (Fig. 6).

We also note that the two Yamato meteorites have 40Ar/39Ar ages that differ by 70 ± 10 Ma (2σ). This age difference is incompatible with the hypothesis that these were fall-paired stones38 (i.e., two parts of a formerly larger meteorite that have become separated, e.g., during atmospheric entry). Despite being found in the same Antarctic field season, there is, however, no a priori scientific reason for why these stones should be fall-paired, particularly when considering that the Yamato meteorite stranding surface is the largest in Antarctica, covering an area of 4000 km2, and that the glaciers which feed into the stranding area extend for a further 500 km upstream39. Yamato 000593 and Yamato 000749 could therefore have fallen anywhere in the catchment area, only to be brought to a similar part of the ice field by the action of Antarctic glaciers.

Our 40Ar/39Ar and cosmogenic exposure ages inform about the provenance of the nakhlites on the surface of Mars, including their ejection crater, and properties of their source volcano. More than seven different Martian craters have been suggested as potential sources for the nakhlites40,41,42. However, when we use the recent re-mapping of the Martian surface by NASA43, we find that only one of these craters is situated in a mid-Amazonian volcanic terrain compatible with our 40Ar/39Ar results (Fig. 1 and Supplementary Table 4). This crater, which is located at 130.799°E, 29.674°N, has preserved ejecta rays42 that are indicative of a recent impact event, which in turn is consistent with the cosmogenic exposure age (10.7 ± 0.8 Ma) obtained for the nakhlites (Fig. 3). This crater has a diameter of 6.5 km, which is large enough for the impact to have had sufficient energy to have excavated and ejected material beyond Mars’ orbit44.

We have investigated high-resolution satellite images from the walls of this crater, which provide clear evidence for multiple layers (Fig. 7); similar layers elsewhere on Mars are interpreted as lava flows35. During an impact event the ejecta that exceeds escape velocity comes from the near-surface of Mars, up to a maximum depth of 0.2 times the impactor’s radius17. The 6.5 km diameter of this crater42 requires the impacting bolide to have a radius of ca. 200 m (Supplementary Table 4). Thus, the spallation zone for this crater is from the near-surface to a depth of 40 m (i.e., 0.2 × 200 m). If the identified crater is not the source of the nakhlites, there are other rayed craters41 situated on Amazonian volcanic terrains that have diameters of up to 10 km, which increases the maximum spallation depth to 66 m (Supplementary Table 4).

Fig. 7
Fig. 7

A potential nakhlite source crater. This crater is located on the Elysium lava plains, to the northwest of the Elysium shield volcano on Mars, at 130.799°E, 29.674°N (Fig. 1). a Overview of the crater, which is 6.5 km in diameter42, large enough to have ejected Martian rocks towards Earth44. THEMIS image V13713007, Band 3, NASA/ASU. Black rectangles indicate the locations for subsequent images. bd Detail of the northwestern, northeastern and southern crater rim, respectively, representing parts of HiRISE image ESP 017997_2100, NASA/JPL/University of Arizona. These images show numerous sub-horizontal layers, which are interpreted as lava flows (e.g., ref. 35 for similar features elsewhere on Mars). White arrows indicate prominent layers; see inset for detailed view. Solar illumination is from the west in all images

If the nakhlite samples analysed span the full spallation depth (near-surface to 40–66 m), then considering the time taken to accumulate the lava sequence (93 ± 12 Ma), approximately 0.4–0.7 m of lava was extruded every 1 Ma. If the nakhlites analysed do not span the full spallation depth, this rate represents an upper bound, whereas if the source crater is located on the volcano flank, or on lava plains, then the calculated rate represents a lower bound, as eruptions are likely to be more voluminous and frequent closer to the centre of an edifice. In all scenarios, the growth rate is three orders of magnitude lower than is observed for a terrestrial plume-derived volcano (e.g., 8400 ± 2600 m Ma−1 at Mauna Kea, Hawai’i)10.

Extrapolating a growth rate of 0.4–0.7 m Ma−1 to the full 6–22 km thickness of the massive Tharsis and Elysium volcanoes7 would necessitate volcanic activity over a timespan exceeding the age of the solar system (>31,000 Ma). Therefore, the eruption rate must have been greater prior to the mid-Amazonian. Both crater counting and planetary heat-flow models support this conclusion, as they demonstrate that the rate of volcanism during the Noachian and Hesperian (4500–3000 Ma) was at least 2–10 times greater than in the Amazonian (<3000 Ma)3, 4, 7. Our data compare favourably with remote-sensing crater-counting studies of Martian volcanoes45,46,47, which indicate that volcanism occurred at much lower rates in the recent past, compared to early in the planet’s history. For example, over the last 300 Ma the maximum effusion rate at the Arisa Mons volcano47 was between 1 and 8 km3 Ma−1—well below the eruption rate of 270 km3 Ma−1 averaged over the 3400 Ma duration of the volcano (Supplementary Table 1).

Our data thus quantify the growth rate of a mid-Amazonian volcano, and robustly show via radioisotopic dating that the minimum lifespan of at least one Martian edifice (93 ± 12 Ma; Fig. 2) far exceeds that of any terrestrial counterpart. This work also resolves the temporal relationships between the nakhlite meteorites, which sample a series of lava flows (Fig. 6), rather than a single thick intrusion/flow18, 36, 37. The high-precision data also provide an ‘absolute’ temporal anchor for the surface of Mars that could underpin a Martian crater counting calibration model, providing the provenance of the nakhlites (i.e., location of their source crater, Fig. 7) can be confirmed.

Methods

Qualitative X-ray element mapping

These data (Fig. 2 and Supplementary Fig. 1) were collected via energy-dispersive spectroscopy on a Carl Zeiss Sigma scanning electron microscope at the University of Glasgow. Samples were carbon-coated, and the electron microscope was operated in high-vacuum mode at 20 kV and ~ 2 nA.

40Ar/39Ar chronology

Samples were prepared at the NERC Argon Isotope Facility, Scottish Universities Environmental Research Centre (SUERC). The meteorites were first gently crushed in an agate mortar and pestle to liberate mineral phases, which were then washed in distilled water to remove dust. Hand-picked chips of groundmass were then wrapped in Cu-foil packets, and loaded in two irradiation vials along with neutron-fluence monitor Hb3gr (standard age of 1081.0 ± 1.2 Ma (1σ)48 and secondary standard GA1550 (standard age of 99.738 ± 0.104 Ma (1σ)48. Samples were then irradiated for 80 h in the Cd-lined TRIGA facility, Oregon State University, USA. After a decay period of 5–9 months, analyses of neutron flux monitors and meteorite samples were undertaken on an MAP 215-50 spectrometer operated in peak-hopping mode, with measured sensitivity of 1.13 × 10−13 mol V−1. Hb3gr crystals were analysed via total-fusion, while meteorite samples were incrementally heated using a using a defocused CO2 laser. The released gases were purified using two SAES GP50 getters with ST101 Zr-Al cartridges, one at room temperature (0 V) and the other at ~ 450 °C (2 V). Isotope extraction, purification, extraction line operation and mass spectrometry were fully automated. Data were corrected for background measurements, mass discrimination and radioactive decay since irradiation using MassSpec software version 8.131. Values used in the 40Ar/39Ar data regression are listed in Supplementary Table 5.

Cosmogenic exposure ages

These analyses were performed on unirradiated aliquots, and were measured both at SUERC and Lawrence Livermore National Laboratory (LLNL). Gas extractions at SUERC followed the procedure described above. At LLNL, whole-rock fragments of Nakhla and Lafayette were loaded into small metal packets made from high-purity Pt–Ir tubes and heated with a 75 W diode laser (λ = 810 ± 10 nm)21. The released argon was purified using four SAES getters (one hot and three cold) and analysed using a Nu Instruments Noblesse mass spectrometer. Samples were analysed statically in peak hopping mode using the axial multiplier detector. Sample analyses were bracketed by analyses of a spike of known abundance and isotopic composition to monitor for time-dependent changes in spectrometer sensitivity and mass discrimination.

Cosmogenic exposure ages were calculated from elemental production rates49. When possible, chemical compositions of each sample were determined by inductively coupled plasma mass spectrometry (ICP-MS) at LLNL (Supplementary Table 3). In two instances (Lafayette and Nakhla aliquot ‘b’), average chemical compositions50 were used for the specific meteorites (see Supplementary Table 3). For 38Ar exposure age calculations, the relative contributions of trapped and cosmogenic Ar were determined by a two-component deconvolution assuming cosmogenic (38Ar/36Ar = 1.54)51 and the trapped component is derived from the Martian atmosphere (38Ar/36Ar = 0.244)52.

To confirm that the small variations in cosmogenic exposure age determined for the different nakhlites (Fig. 3) are not responsible for the differences in 40Ar/39Ar ages across the group (Fig. 6), we also calculated the 40Ar/39Ar ages using the weighted mean cosmogenic exposure age of 10.7 ± 0.8 Ma. These calculations (Supplementary Fig. 3) demonstrate that the plateau age for each meteorite is insensitive to small (1–2 Ma) variations in cosmogenic exposure age, and that the ca. 90 Ma age difference between Lafayette and Yamato 000749 is robust (Supplementary Fig. 3).

Data availability

The authors declare that all data supporting the findings of this study are included in this published article (and its supplementary information files).

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References

  1. 1.

    Gurnis, M. A reassessment of the heat transport by variable viscoscity convection with plates and lids. Geophys. Res. Lett. 16, 179–182 (1989).

  2. 2.

    Morgan, W. J. Convection plumes in the lower mantle. Nature 230, 42–43 (1971).

  3. 3.

    Sleep, N. H. Martian plate tectonics. J. Geophys. Res. Planets 99, 5639–5655 (1994).

  4. 4.

    Grott, M. et al. Long-term evolution of the Martian crust-mantle system. Space Sci. Rev. 174, 49–111 (2012).

  5. 5.

    Wenzel, M. J. Tharsis as a consequence of Mars’ dichotomy and layered mantle. Geophys. Res. Lett. 31, L04702 (2004).

  6. 6.

    Ramalho, R. S. et al. Emergence and evolution of Santa Maria Island (Azores)—the conundrum of uplifted islands revisited. Geol. Soc. Amer. Bull. 129, 372–390 (2016).

  7. 7.

    Werner, S. C. The global Martian volcanic evolutionary history. Icarus 201, 44–68 (2009).

  8. 8.

    Plescia, J. B. Morphometric properties of Martian volcanoes. J. Geophys. Res. 109, E03003 (2004).

  9. 9.

    Platz, T., Byrne, P. K., Massironi, M. & Hiesinger, H. Volcanism and tectonism across the inner solar system: an overview. Geol. Soc. Lond. Spec. Publ. 401, 1–56 (2014).

  10. 10.

    Jourdan, F., Sharp, R. P. & Renne, P. R. 40Ar/39Ar ages for deep (~3.3 km) samples from the Hawaii scientific drilling project, Mauna Kea volcano, Hawaii. Geochem. Geophys. Geosyst. 13, Q05004 (2012).

  11. 11.

    Hartmann, W. K. & Neukum, G. Cratering chronology and the evolution of Mars. Space Sci. Rev. 96, 165–194 (2001).

  12. 12.

    Kerr, R. A. Who can read the Martian clock? Science 312, 1132–1133 (2006).

  13. 13.

    Treiman, A. H. The nakhlite meteorites: augite-rich igneous rocks from Mars. Chem. Erde – Geochem. 65, 203–270 (2005).

  14. 14.

    Righter, M., Lapen, T. J., Andreasen, R. & Irving, A. J. Lu-Hf and Sm-Nd isotopic studies of nakhlite Northwest Africa 10153. Lunar Planet. Sci. Conf. XLVII, 2780 (2016).

  15. 15.

    Jambon, A. et al. Northwest Africa 5790: revisiting nakhlite petrogenesis. Geochim. Cosmochim. Acta 190, 191–212 (2016).

  16. 16.

    Herzog, G. F. & Caffee, M. W. in Treatise on Geochemistry 2nd edn, Vol. 1, Ch. 1.13, 419–454 (Elsevier, 2014).

  17. 17.

    Fritz, J., Artemieva, N. & Greshake, A. Ejection of Martian meteorites. Meteorit. Planet. Sci. 40, 1393–1411 (2005).

  18. 18.

    Mikouchi, T., Makishima, J., Kurihara, T., Hoffmann, V. H. & Miyamoto, M. Relative burial depth of Nakhlites revisited. Lunar Planet. Sci. Conf. XLIII, 2363 (2012).

  19. 19.

    Bogard, D. D. & Garrison, D. H. Argon-39-argon-40 “ages” and trapped argon in Martian shergottites, Chassigny, and Allan Hills 84001. Meteorit. Planet. Sci. 34, 451–473 (1999).

  20. 20.

    Park, J., Bogard, D. D., Nyquist, L. E., Garrison, D. H. & Mikouchi, T. Ar–Ar ages and trapped Ar components in Martian shergottites RBT 04262 and LAR 06319. Geochim. Cosmochim. Acta 121, 546–570 (2013).

  21. 21.

    Cassata, W. S. & Borg, L. E. A new approach to cosmogenic corrections in 40Ar/39Ar chronometry: implications for the ages of Martian meteorites. Geochim. Cosmochim. Acta 187, 279–293 (2016).

  22. 22.

    Cartwright, J. A., Gilmour, J. D. & Burgess, R. Martian fluid and Martian weathering signatures identified in Nakhla, NWA 998 and MIL 03346 by halogen and noble gas analysis. Geochim. Cosmochim. Acta 105, 255–293 (2013).

  23. 23.

    Fleck, R. J., Sutter, J. F. & Elliot, D. H. Interpretation of discordant 40Ar/39Ar age-spectra of Mesozoic tholeiites from Antarctica. Geochim. Cosmochim. Acta 41, 15–32 (1977).

  24. 24.

    McDougall, I. & Harrison, T. M. Geochronology and Thermochronology by the 40 Ar/ 39 Ar Method 2nd edn, 261 (Oxford University Press, 1999).

  25. 25.

    VanLaningham, S. & Mark, D. F. Step heating of 40Ar/39Ar standard mineral mixtures: investigation of a fine-grained bulk sediment provenance tool. Geochim. Cosmochim. Acta 75, 2324–2335 (2011).

  26. 26.

    Cassata, W. S., Shuster, D. L., Renne, P. R. & Weiss, B. P. Evidence for shock heating and constraints on Martian surface temperatures revealed by 40Ar/39Ar thermochronometry of Martian meteorites. Geochim. Cosmochim. Acta 74, 6900–6920 (2010).

  27. 27.

    Bogard, D. D. & Garrison, D. H. Ar-Ar dating of Martian chassignites, NWA2737 and Chassigny, and nakhlite MIL03346. Lunar Planet. Sci. Conf. XXXVII, 1108 (2006).

  28. 28.

    McSween, H. Y. & McLennan, S. M. in Treatise on Geochemistry 2nd edn, Vol. 2, Ch. 2.10, 251–300 (Elsevier, 2014).

  29. 29.

    Mahaffy, P. R. et al. Abundance and isotopic composition of gases in the Martian atmosphere from the Curiosity Rover. Science 341, 263–266 (2013).

  30. 30.

    Bogard, D. D., Clayton, R. N., Marti, K., Owen, T. & Turner, G. Martian volatiles: isotopic composition, origin, and evolution. Space Sci. Rev. 96, 425–458 (2001).

  31. 31.

    Stuart, F. M., Mark, D. F., Gandanger, P. & McConville, P. Earth-atmosphere evolution based on new determination of Devonian atmosphere Ar isotopic composition. Earth Planet. Sci. Lett. 446, 21–26 (2016).

  32. 32.

    Cassata, W. S., Shuster, D. L., Renne, P. R. & Weiss, B. P. Trapped Ar isotopes in meteorite ALH 84001 indicate Mars did not have a thick ancient atmosphere. Icarus 221, 461–465 (2012).

  33. 33.

    Shih, C. Y., Nyquist, L. E. & Reese, Y. Rb-Sr and Sm-Nd isotopic studies of Antarctic nakhlite MIL 03346. Lunar Planet. Sci. Conf. XXXVII, 1701 (2006).

  34. 34.

    Basilevskaya, E. A. & Neukum, G. The Olympus volcano on Mars: geometry and characteristics of lava flows. Solar System Res. 40, 375–383 (2006).

  35. 35.

    Keszthelyi, L. et al. High Resolution Imaging Science Experiment (HiRISE) images of volcanic terrains from the first 6 months of the Mars Reconnaissance Orbiter primary science phase. J. Geophys. Res. 113, E04005 (2008).

  36. 36.

    Mikouchi, T., McKay, G. & Miyamoto, M. Mineralogy of nakhlite Martian meteorites: implications for their relative burial depths. Gen. Meeting Int. Mineralog. Assoc. Conf., 19 (2006).

  37. 37.

    Mikouchi, T., Miyamoto, M., Koizumi, E., Makishima, J. & McKay, G. Relative burial depths of Nakhlites: an update. Lunar Planet. Sci. Conf. XXXVII, 1865 (2006).

  38. 38.

    Misawa, K., Kojima, H., Imae, N. & Nakamura, N. The Yamato nakhlite consortium. Antarct. Meteorite Res. 16, 1–12 (2003).

  39. 39.

    Cassidy, W., Harvey, R., Schutt, J., Delisle, G. & Yanai, K. The meteorite collection sites of Antarctica. Meteoritics 27, 490–525 (1992).

  40. 40.

    Harvey, R. P. & Hamilton, V. E. Syrtis Major as the source region of the nakhlite/chassigny group of Martian meteorites: implications for the geological history of Mars. Lunar Planet. Sci. Conf. XXXVI, 1019 (2005).

  41. 41.

    Tornabene, L. L. et al. Identification of large (2–10 km) rayed craters on Mars in THEMIS thermal infrared images: implications for possible Martian meteorite source regions. J. Geophys. Res. 111, E10006 (2006).

  42. 42.

    Kereszturi, A. & Chatzitheodoridis, E. Searching for the source crater of nakhlite meteorites. Orig. Life. Evol. Biosph. 46, 455–471 (2016).

  43. 43.

    Tanaka, K. L. et al. Geologic map of Mars. U.S. Geological Survey Scientific Investigations Map 3292 (2014).

  44. 44.

    Head, J. N., Melosh, H. J. & Ivanov, B. A. Martian meteorite launch: high-speed ejecta from small craters. Science 298, 1752–1756 (2002).

  45. 45.

    Isherwood, R. J., Jozwiak, L. M., Jansen, J. C. & Andrews-Hanna, J. C. The volcanic history of Olympus Mons from paleo-topography and flexural modeling. Earth. Planet. Sci. Lett. 363, 88–96 (2013).

  46. 46.

    Chadwick, J., McGovern, P., Simpson, M. & Reeves, A. Late Amazonian subsidence and magmatism of Olympus Mons, Mars. J. Geophys. Res. Planets 120, 1585–1595 (2015).

  47. 47.

    Richardson, J. A., Wilson, J. A., Connor, C. B., Bleacher, J. E. & Kiyosug, K. Recurrence rate and magma effusion rate for the latest volcanism on Arsia Mons, Mars. Earth. Planet Sci. Lett. 458, 170–178 (2017).

  48. 48.

    Renne, P. R., Balco, G., Ludwig, K. R., Mundil, R. & Min, K. Response to the comment by W.H. Schwarz et al. on “joint determination of 40K decay constants and 40Ar*/40K for the Fish Canyon sanidine standard, and improved accuracy for 40Ar/39Ar geochronology” by Paul R. Renne et al. (2010). Geochim. Cosmochim. Acta 75, 5097–5100 (2011).

  49. 49.

    Eugster, O. & Michel, T. Common asteroid break-up events of eucrites, diogenites, and howardites and cosmic-ray production rates for noble gases in achondrites. Geochim. Cosmochim. Acta 59, 177–199 (1995).

  50. 50.

    Lodders, K. A survey of shergottite, nakhlite and chassigny meteorites whole-rock compositions. Meteorit. Planet. Sci. 33, A183–A190 (1998).

  51. 51.

    Wieler, R. Cosmic-ray-produced noble gases in meteorites. Rev. Mineral. Geochem 47, 125–170 (2002).

  52. 52.

    Wiens, R. C., Becker, R. H. & Pepin, R. O. The case for a Martian origin of the shergottites, II. Trapped and indigenous gas components in EETA 79001 glass. Earth Planet. Sci. Lett. 77, 149–158 (1986).

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Acknowledgements

We thank the following institutions for providing the meteorite samples: Smithsonian Museum, NASA Meteorite Working Group, Natural History Museum London, Macovich Collection and the Japanese Antarctic Meteorite Research Centre. This work was funded by the Science and Technology Facilities Council (grants ST/H002472/1, ST/H002960/1 and ST/K000918/1 to D.F.M. and M.R.L.) and the NASA Mars Fundamental Research Program (grant NNH14AX56I to W.S.C.). Portions of this work were performed under the auspices of the U.S. Department of Energy by Lawrence Livermore National Laboratory under Contract DE-AC52-07NA27344. NERC are thanked for continued funding of the Argon Isotope Facility at SUERC. R. Dymock and J. Imlach (SUERC), P. Lindgren and P. Chung (University of Glasgow) assisted with 40Ar/39Ar and scanning electron microscopy, respectively. We thank F. Jourdan and W.S. Kiefer for reviews.

Author information

Affiliations

  1. Isotope Geoscience Unit, Scottish Universities Environmental Research Centre (SUERC), Rankine Avenue, East Kilbride, G75 0QF, UK

    • Benjamin E. Cohen
    • , Darren F. Mark
    •  & Tim Tomkinson
  2. School of Geographical and Earth Sciences, University of Glasgow, Glasgow, G12 8QQ, UK

    • Benjamin E. Cohen
    •  & Martin R. Lee
  3. Department of Earth & Environmental Science, University of St Andrews, St Andrews, KY16 9AJ, UK

    • Darren F. Mark
  4. Nuclear & Chemical Sciences Division, Lawrence Livermore National Laboratory, 7000 East Avenue (L-231), Livermore, CA, 94550, USA

    • William S. Cassata
  5. Department of Earth Sciences, The Natural History Museum, London, SW7 5BD, UK

    • Caroline L. Smith

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Contributions

The project was developed by D.F.M., M.R.L. and B.E.C.; samples were acquired by C.L.S., D.F.M. and M.R.L.; samples were prepared by T.T., D.F.M., B.E.C. and W.S.C.; analysed by D.F.M., B.E.C. and W.S.C. Data was interpreted and manuscript prepared by B.E.C., D.F.M., W.S.C. and M.R.L., with small contributions from other authors.

Competing interests

The authors declare no competing financial interests.

Corresponding author

Correspondence to Benjamin E. Cohen.

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