Introduction and background

Present-day Mars is a cold, hyper-arid desert; liquid water is unstable at the surface under the thin (~6 mbar) atmosphere. Away from the polar caps, ice is also unstable at the surface and will sublimate if exposed. Despite this, abundant ice exists in Mars' subsurface down to latitudes of ~30°N/S, both as ground ice and massive glacial ice (e.g. Butcher, Reference Butcher2022 and references therein). Putative buried glaciers (termed ‘viscous flow features’, VFFs) in Mars' mid latitudes (e.g. Head and others, Reference Head2005; Holt and others, Reference Holt2008) are thought to have formed 10s to 100s Myr ago due to climate changes driven by large cyclical variations in Mars' spin-axis obliquity (e.g. Madeleine and others, Reference Madeleine2009). A protective lithic cover has allowed the glaciers to be preserved into the present day.

It is thought that Mars' ‘Amazonian’ period (3 Ga to present) was, in general, similarly cold and dry to the present day (current mean annual temperature ~210 K). Mars' geomorphology suggests an extremely limited role of liquid water in Amazonian environments (e.g. Carr and Head, Reference Carr and Head2010), leading to an informal baseline assumption that the mid-to-late-Amazonian-aged VFFs have always been cold-based. However, targeted analyses of individual glacial landsystems paint a more complex picture of VFF thermal histories, and thus an expanded range of environmental and glaciological conditions in Mars' geologically-recent past. For example, evidence of glacial streamlining has been identified in some locations (e.g. Hubbard and others, Reference Hubbard, Milliken, Kargel, Limaye and Souness2011; Gallagher and others, Reference Gallagher, Butcher, Balme, Smith and Arnold2021). However, Mars does not host widespread streamlined terrains like those generated by warm-based ice masses on Earth.

Theoretically, under lower Martian gravity, subglacial drainage might develop towards efficient channelised drainage more readily than on Earth, reducing basal water pressures and inhibiting sliding and bedform streamlining (Grau Galofre and others, Reference Grau Galofre, Whipple, Christensen and Conway2022). Therefore, Grau Galofre (Reference Grau Galofre, Whipple, Christensen and Conway2022) and others posit that the most common indicator landforms of warm-based glaciation on Mars could be those formed by channelized subglacial meltwater, including eskers. This is consistent with a growing number of ‘candidate glacier-linked eskers’ identified emerging from, or geomorphologically connected to, VFFs (Gallagher and Balme, Reference Gallagher and Balme2015; Butcher and others, Reference Butcher2017, Reference Butcher2020, Reference Butcher2021; Woodley and others, Reference Woodley2022).

Candidate eskers linked to mid-latitude buried glaciers on Mars

Using ~6 m/pixel orbital Context Camera (CTX) images (see Supplementary Table S1; Malin and others, Reference Malin2007), Gallagher and Balme (Reference Gallagher and Balme2015) identified a candidate glacier-linked esker assemblage in the foreland of a VFF occupying a tectonic graben in Phlegra Montes, a mountain chain in Mars' northern mid-latitudes (Figs 1a and b). The candidate esker assemblage is connected to the glacier by a corridor which appears similar to proglacial fluvial systems on Earth (Fig 1c; Gallagher and Balme, Reference Gallagher and Balme2015). Butcher and others (Reference Butcher2017) subsequently identified a candidate esker (Fig 1d) emerging from a VFF in NW Tempe Terra, a volcano-tectonic province ~5000 km east of Phlegra Montes (Fig 1e). Like the candidate esker assemblage in Phlegra Montes, it occupies a glaciated graben (Fig 1e). Woodley and others (Reference Woodley2022) identified two additional candidate glacier-linked eskers (Figs 1f and g) in the same system of grabens where it extends into W Tempe Terra (Fig 1e). Butcher and others (Reference Butcher2021) also found that at least one morphological subpopulation of sinuous ridges associated with a VFF within Chukhung crater (in central Tempe Terra, Fig 1e) is best explained as eskers. Chukhung crater sits between branches of a major volcano-tectonic rift system (Fig 1e).

Fig. 1.

a. A buried glacier in Phlegra Montes connected to the candidate esker assemblage identified by Gallagher and Balme (Reference Gallagher and Balme2015) (shown in b, 162.97°E, 32.68°N) by a corridor of landforms similar to proglacial zones on Earth (shown in c, including channels, thermokarst-like terrain and dead ice topography). d. Candidate glacier-linked esker (83.06°W, 46.17°N; Butcher and others (Reference Butcher2017)) emerging from a buried glacier in NW Tempe Terra. e. Mars Orbiter Laser Altimeter (MOLA) elevation map showing candidate glacier-linked esker sites in the Tempe Terra region (yellow triangles), including Chukhung crater (72.42°W, 38.47°N; Butcher and others (Reference Butcher2021)). Inset global elevation map shows locations of panel e (black polygon) and Phlegra Montes (red triangle). f and g. Candidate glacier-linked eskers in W Tempe Terra (84.387°W, 43.772°N; and 83.295°W, 44.334°N; Woodley and others (Reference Woodley2022)). Panels a, c, d, f and g are CTX images. Panel b is a High Resolution Imaging Science Experiment (HiRISE) image. See Supplementary Table S2 for image codes.

Planetary surface ages are estimated using the size-frequency distributions of impact craters. The candidate glacier-linked eskers are too small to extract direct age estimates but their minimum ages can be estimated from impact craters on their parent glaciers. While affected by substantial uncertainties, all return ages firmly in the mid-to-late Amazonian (110 Ma from Butcher and others, Reference Butcher2017; 150 Ma from Gallagher and Balme, Reference Gallagher and Balme2015; 220 Ma from Woodley and others, Reference Woodley2022; and 330 Ma from Butcher and others, Reference Butcher2021).

Open questions and research directions

Discoveries of candidate eskers associated with buried glaciers in Mars' mid latitudes raise numerous questions. Those summarised below are far from an exhaustive list.

Identifications of a handful of glacier-linked eskers do not necessarily warrant global-scale re-imagination of the cold, dry climate of Amazonian Mars (3 Ga to present). However, they demonstrate that we have an incomplete understanding of the range of thermal conditions during the Amazonian. We also have an incomplete understanding of fundamentals such as ice mass-balance, which strongly influence glacier thermal regime. For example, modelling suggests that Mars' low atmospheric pressure could have caused preferential ice accumulation in topographic lows, rather than at higher altitudes (Fastook and others, Reference Fastook, Head, Marchant and Forget2008).

The similarity in geologic settings between the candidate glacier-linked eskers identified to date (within or associated with tectonic grabens/rifts) suggests that geothermal heating could have driven basal melting. This hypothesis was posited by Gallagher and Balme (Reference Gallagher and Balme2015) and subsequently explored with a 1D thermal model by Butcher and others (Reference Butcher2017), which considered strain heating for the first time. Strain heating has a highly non-linear temperature dependence, and could be enhanced by geothermal heat and/or by ice-flow deformation in high-relief settings, such as grabens. Butcher and others (Reference Butcher2017) found that strain heating provided up to 14.5 K of additional heating, and modelled basal temperatures approached 273 K for local mean annual surface temperatures >205 K (from current ~190 K in mid latitudes), ice thicknesses >900 m, and geothermal heat fluxes >50 mWm^-2. Simplified global models predict that Mars' present-day average geothermal heat flux is ~23–27 mWm⁻², reaching ~50 mWm⁻² in confined areas (Plesa and others, Reference Plesa2016). Thus, it is conceivable that localised, late-stage geothermal activity (e.g. magmatic intrusions), combined with strain heating, drove basal melting. A conservative scenario for esker formation is therefore one of localised and transient polythermal glaciation, with geothermal and strain heating driving the accumulation of subglacial meltwater, which was initially prevented from draining due to confinement by cold-based marginal ice. Eventual water over-pressurisation could have driven rapid drainage towards the ice margin (either subglacially, or by routing upwards into an englacial position) to form eskers (e.g. Butcher and others, Reference Butcher2017).

Woodley and others (Reference Woodley2022) considered the hypothesis that regional climate change could explain the discoveries of multiple candidate glacier-linked eskers in Tempe Terra, over a region spanning hundreds of kilometres (Fig 1e) (Butcher and others, Reference Butcher2017, Reference Butcher2021; Woodley and others, Reference Woodley2022). They suggest that multiple, spatially distributed but localised geothermal heating events in this extensively tectonised region remain the strongest explanation, owing to the lack of associated evidence for past supraglacial melting. However, arguably, any supraglacial channels temporally associated with esker formation would have been erased by the kilometres-scale ice retreat that has since occurred.

Harder to explain without invoking substantial climate change are the channels, consistent with proglacial runoff (Fig 1c), which now separate the candidate esker in Phlegra Montes from its parent glacier (Gallagher and Balme, Reference Gallagher and Balme2015). Furthermore, Gallagher and others (Reference Gallagher, Butcher, Balme, Smith and Arnold2021) also identified regionally-extensive evidence for warm-based glacial erosion in the wider Phlegra Montes region, including zones of areal scour, candidate tunnel valleys, overdeepenings and groove-channel systems. If this Phlegra Montes landsystem is genetically related to the candidate glacier-linked esker, it complicates the hypothesis that esker formation was controlled by localised geothermal heating, suggesting more spatially extensive driver(s) of melting, for example a regional climate change and/or a regional geothermal hotspot (e.g. Broquet and Andrews-Hanna, Reference Broquet and Andrews-Hanna2022).

A further unknown is the degree to which salts contributed to basal melting of VFFs. Salts detected on Mars, such as Na, Mg or Ca perchlorate (Hecht and others, Reference Hecht2009) can reduce the melting point by tens of Kelvin. Mg perchlorate hydrate can also weaken ice, potentially enhancing ice flow and associated strain heating (Lenferink and others, Reference Lenferink, Durham, Stern and Pathare2013). Thus, salts could have substantially reduced the requisite heating for basal melting; however, it is not known whether they are/were present beneath VFFs, and in sufficient concentrations to influence thermal regimes and increase melt to levels needed for subglacial channelisation and esker formation.

To better understand the environmental implications of glacier-linked eskers (Q1), it is necessary to constrain their global-scale abundance and distribution. Hemispheric-to-global-scale constraints on esker distributions would permit comparisons to models of palaeoclimate and geothermal heat flux, and hence assessment of potential environmental drivers of melting. Identifications of glacier-linked eskers are rare (5 sites) compared to the abundance of mid-latitude VFFs (>12 000; Levy and others, Reference Levy, Fassett, Head, Schwartz and Watters2014; Brough and others, Reference Brough, Hubbard and Hubbard2019). However, the vast majority of Mars' glacial landscapes have not been analysed in detail, and there is a wealth of imaging data left to explore, including near-global coverage of ~6 m pixel⁻¹ CTX images (Malin and others, Reference Malin2007), and more localised 25–50 cm pixel⁻¹ HiRISE images (McEwen and others, Reference McEwen2007). Supplementary Table S1 describes key image and elevation datasets, with data-access links, and Supplementary Information 1 provides an introductory tutorial for exploring orbital images of Mars.

A key challenge for addressing Q2 is reliably distinguishing between eskers and morphologically similar landforms of different origin. Inverted fluvial palaeochannels are ridges comprising resistant infills of fluvial channels or channel belts, exhumed by erosion of less resistant surrounding materials (e.g. Williams and others, Reference Williams, Chidsey, Eby, Willis, Hylland, Clark and Chidsey2007). While typical inverted fluvial palaeochannels can appear distinctive from typical eskers, their morphological ranges overlap, complicating esker identification on Mars where landsystems consistent with both origins co-exist (e.g. in Chukhung crater; Butcher and others, Reference Butcher2021).

Several studies exploring esker origins for sinuous ridges on Mars have included comparisons to the planform morphometries (e.g. length, sinuosity, fragmentation) of >20 000 eskers deposited by the Laurentide Ice Sheet on Earth (Storrar and others, Reference Storrar, Stokes and Evans2014), identifying sinuosity as a particular source of similarity (Butcher and others, Reference Butcher, Conway and Arnold2016; Butcher, Reference Butcher2019; Woodley and others, Reference Woodley2022). 3D (e.g. height and width) comparisons with Earth's eskers (e.g. Butcher and others, Reference Butcher, Conway and Arnold2016; Butcher, Reference Butcher2019) are more limited as datasets from Earth are currently restricted to qualitative descriptions, or measurements of individual eskers (e.g. Perkins and others, Reference Perkins, Brennand and Burke2016). The morphometries of eskers associated with Earth's ice caps and valley glaciers (e.g. Storrar and others, Reference Storrar, Evans, Stokes and Ewertowski2015) are similarly understudied, but could be more appropriate analogues, in both scale and setting, for glacier-linked eskers on Mars. Large-sample morphometric statistics of a range of terrestrial analogue landforms, including those which could provide alternative explanations for sinuous ridges (e.g. inverted palaeochannels), would greatly enhance our ability to explore origin hypotheses for glacier-linked sinuous ridges on Mars.

Mineralogy could also help to distinguish between eskers and sinuous ridges of different origin. For example, it can reveal evidence for the involvement and residence times (Q3) of liquid water. Several studies also suggest that cold and icy weathering could have produced amorphous materials observed on Mars, such as the mineraloids allophane and hydrated silica (e.g. Hallet, Reference Hallet1975; Rutledge and others, Reference Rutledge2018; Rampe and others, Reference Rampe2022). There are numerous orbital infrared datasets (Supplementary Table S3) which can help identify and map mineral classes, at varying spatial and spectral scales, and thereby interpret whether sinuous ridge formation involved liquid water and/or occurred under climate conditions consistent with glacial origins.

To improve confidence in esker identifications on Mars (Q2), and to constrain their palaeoenvironmental/glaciological implications (Q1), it is necessary to understand how eskers on Mars and Earth might differ morphometrically and sedimentologically, for example due to differences in subglacial hydrology and sedimentation arising from the difference in gravity and ice rheology. The candidate glacier-linked eskers measured to date approach the width-height ratios of eskers on Earth, but are typically wider relative to their heights (e.g. Butcher, Reference Butcher2019; Butcher and others, Reference Butcher2020; Woodley and others, Reference Woodley2022). It is not yet understood whether such differences weaken the esker hypothesis, or could be explained by fundamental differences in esker formation dynamics (e.g. due to gravity or ice rheology) and/or degradation states (e.g. due to differences in post-depositional exposure time and erosion rates) relative to Earth (Butcher, Reference Butcher2019; Woodley and others, Reference Woodley2022).

Some studies have related the morphometries of eskers on both Earth and Mars to the drainage dynamics that formed them (e.g. Butcher and others, Reference Butcher, Conway and Arnold2016, Reference Butcher2020; Perkins and others, Reference Perkins, Brennand and Burke2016). By analogy to terrestrial eskers, Butcher and others (Reference Butcher2020) suggested that the complex ‘stacked’ morphology of the candidate glacier-linked esker in NW Tempe Terra could result from spatio-temporal variations in sediment-discharge dynamics, either in a single drainage episode, or multiple episodes separated by ice retreat. Analyses of esker sedimentary architecture at exposed sections and/or using ground-penetrating radar have enhanced efforts to reconstruct esker-forming drainage events on Earth (e.g. Perkins and others, Reference Perkins, Brennand and Burke2016) but are not possible with the current instruments at Mars. Esker sedimentation on Earth remains relatively poorly understood, as does its relationship to subglacial hydrology and the morphometry of the resulting landforms (e.g. Stoker and others, Reference Stoker2021). Furthermore, despite a considerable amount of research into eskers formed during the last deglaciation on Earth, fewer studies focus on esker sedimentation at contemporary glacier margins (e.g. Burke and others, Reference Burke, Woodward, Russell, Fleisher and Bailey2008, Reference Burke, Woodward, Russell, Fleisher and Bailey2010; Storrar and others, Reference Storrar, Evans, Stokes and Ewertowski2015). These eskers are important analogues for Mars, and exhibit morphological differences to their large ice sheet counterparts.

Recent advances demonstrate the potential utility of new esker sedimentation models (Beaud and others, Reference Beaud, Flowers and Venditti2018; Hewitt and Creyts, Reference Hewitt and Creyts2019) for relating sediment deposition in subglacial conduits to parameters such as bed slope (Stevens and others, Reference Stevens2022). As esker sedimentation modelling advances, it could help explore the dynamics of esker sedimentation on Mars, including potential morphological/sedimentological differences arising from differences in gravity and ice rheology.

The ultimate fate of esker-forming meltwater on Amazonian Mars remains uncertain. Did it pond, run off, refreeze, percolate into the ground and/or rapidly evaporate/boil? Did it accumulate in standing (perhaps ice-covered) bodies of water such as proglacial lakes or ponds? Constraining the contributions of these processes would help to answer Q1 and Q3 because the behaviour of liquid water upon exiting the subglacial environment would have been dependent on factors such as climate and atmospheric pressure and the duration, frequency and discharge of esker-forming drainage.

Under atmospheric pressures similar to present day Mars, liquid water would be stable in a pressurised, water-filled subglacial conduit, but would become unstable upon reaching the ice margin. Laboratory simulations suggest that metastable liquid water flows could persist over short distances under Mars' atmospheric pressure (Massé and others, Reference Massé2016). Their simulated behaviours and geomorphic imprints are quite different to flows under Earth's atmospheric pressure (e.g. Massé and others, Reference Massé2016; Brož and others, Reference Brož2020), but it is unknown if/how they would further differ for discharges and sediment grain-sizes typical of esker-forming flows. Since eskers on Earth are often associated with high-discharge meltwater drainage, we might expect sediment-laden meltwater on Mars to be transported for some distance beyond the ice margin before boiling, percolating into the regolith and/or refreezing (see e.g. Brož and others, Reference Brož2020). A fan-shaped system of distributary ridges at the terminus of a candidate glacier-linked esker identified by Woodley and others (Reference Woodley2022) (Fig 1f) could indicate meltwater and sediment dispersal over a distance of ~500 m at the outlet of a subglacial (or englacial) conduit. However, eskers on Earth commonly terminate abruptly, so esker-terminal fans are not expected in all cases and, indeed, are not always observed on Mars.

Mars’ mid-latitude glacial cycles are thought to have been linked to large variations in planetary obliquity which drove global-scale changes to climate, aerosol and volatile cycles (e.g. Madeleine and others, Reference Madeleine2009), but many uncertainties remain (e.g. Forget and others, Reference Forget, Byrne, Head, Mischna, Schörghofer, Haberle, Clancy, Forget, Smith and Zurek2017). Mars’ current atmospheric pressure is very close to the triple point of water. If glacier-linked eskers are related to changes in atmospheric conditions relative to the present day, it is possible that liquid water would have been stable upon exiting subglacial conduits. In this case, it would be necessary to constrain the relative contributions of runoff, ponding, percolation, refreezing and/or evaporation to the fate of esker-forming meltwater. Morphological analyses of the terminal zones of candidate eskers, and the terrains beyond them, will be important to understand the fate of subglacial meltwater upon entering the proglacial zone.