Subsurface water and clay mineral formation during the early history of Mars

By Bethany L. Ehlmann, J. F. Mustard, Scott L. Murchie, J. Bibring, A. Meunier, A. Fraeman, Yves Langevin. Nature, 2011

815 citations recorded by the source corpus.

Subfields: Aerospace Engineering, Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/1e281818a193b48a9e7dcbdc460483271161bc1c

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Aerospace Engineering

In Astronomy and Astrophysics

Citations in the corpus

Geologic Constraints on Early Mars Climate (2018, background): “In summary, climate-driven surface aqueous alteration on Mars had shut down in most places by ~3.4 Ga (Ehlmann et al. 2011a, Edwards & Ehlmann 2014).”
Mineralogy of the Martian Surface (2014, background): “…the major processes affecting the mineralogic composition of Mars and the ages of large-scale compositional units. aluminum clay minerals in units dating from near the Noachian–Hesperian boundary indicate a late Noachian climate optimum or preservation bias (Figure 6) (e.g., Ehlmann et al. 2011)?”
The Climate of Early Mars (2016, methodology): “Recently, however, it has been argued that in most cases their mineralogy may best represent subsurface formation in geothermally heated, water-poor systems (Ehlmann et al. 2011).”
3D modelling of the early Martian Climate under a denser CO2 atmosphere: Temperatures and CO2 ice clouds. (2012, background): “A wide range of possible climates is explored using various values of obliquities, orbital parameters, cloud microphysic parameters, atmospheric dust loading, and surface properties.”
Petrology on Mars (2015, background): “Noachian geothermal gradients based solely on heat-producing radioactive elements are not high enough to produce the observed mineral assemblages at these depths, so additional heat supplied by geothermal sources seems likely (Ehlmann et al. 2011; McSween et al. 2014).”
Heterogeneous distribution of H2O in the Martian interior: Implications for the abundance of H2O in depleted and enriched mantle sources (2016, background): “…1979; Carr 1996; Baker 2001; Squyres et al. 2004; Haskin et al. 2005; McSween 2006; McEwen et al. 2007; Mustard et al. 2008; Smith et al. 2009; Ehlmann et al. 2011; Grotzinger et al. 2014), but the timing and extent to which this water participated in a global hydrologic cycle is still open…”