On the orbital forcing of Martian water and CO2 cycles: A general circulation model study with simplified volatile schemes

By M. Mischna, Mark Richardson, Robert J. Wilson, Dan J. McCleese. 2003

260 citations recorded by the source corpus.

Subfields: Aerospace Engineering, Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/0e8a23c434022d09ac7af7c4786f4f083231a672

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In Aerospace Engineering

In Astronomy and Astrophysics

Citations in the corpus

The Climate of Early Mars (2016, background): “Mars’ obliquity has varied significantly throughout the Amazonian, however (Laskar & Robutel 1993), and at high obliquities ice migration to equatorial (Mischna et al. 2003; Forget et al. 2006) and mid-latitude (Madeleine et al. 2009) regions is predicted.”
Extensive valley glacier deposits in the northern mid-latitudes of Mars: Evidence for Late Amazonian obliquity-driven climate change (2006, background): “These studies [4–7] show that at obliquities of 458 or more, water vapor mobilized from the polar regions is redistributed at mid-latitudes, is stable there as ice, and will accumulate if obliquity remains at these values.”
The Polar Deposits of Mars (2009, background): “The associated insolation increase (Figure 4f ) could allow the annual ablation of decimeters of ice from the polar deposits, which, in the absence of mitigating effects, would destroy both PLDs in ∼104 years ( Jakosky et al. 1995; Mischna et al. 2003; 546 Byrne A nn u.”
The Modern Near-Surface Martian Climate: A Review of In-situ Meteorological Data from Viking to Curiosity (2017, background): “…by which water is exchanged between the surface and the atmosphere through various processes, and then redistributed in the atmosphere by atmospheric circulations (Jakosky and Farmer 1982; Jakosky 1985; Jakosky and Haberle 1992; Houben et al. 1997; Richardson and Wilson 2002; Mischna et al. 2003).”
Impact crater formation in icy layered terrains on Mars (2006, background): “Therefore, the cratering record implies that near-surface icy layers are widespread on Mars.”
Ground ice at the Phoenix Landing Site: Stability state and origin (2009, background): “[34] Subaerial deposition and interannual accumulation of water frost or snow during a geologically recent climate cycle, in response to orbit oscillations, has been suggested to occur in some regions of Mars based on climate models [e.g., Mischna et al., 2003; Levrard et al., 2004].”
North polar cap of Mars: Polar layered deposit characterization and identification of a fundamental climate signal (2005, unknown): “…dust storm activity and decreased ice deposition and retention during periods of mean high obliquity [e.g., Jakosky et al., 1995; Richardson and Wilson, 2002; Haberle et al., 2003; Mischna et al., 2003] could produce a higher dust-to-ice ratio and a general darkening of the resulting deposits.”
Long term evolution and chaotic diffusion of the insolation quantities of Mars (2004, unknown): “…parameters close to the “standard model” shows that large increases in summer insolation may cause dynamical instability of the polar caps and an intensive sublimation multiplying global atmospheric humidity by a factor ∼ 50 (Jakosky et al. 1995, Richardson and Wilson 2002, Mischna et al. 2003).”
Amazonian northern mid-latitude glaciation on Mars: A proposed climate scenario (2009, background): “Concurrently, developments in climate modeling are providing robust tools to explore this past water cycle (Haberle et al., 2000; Mischna et al., 2003; Levrard et al., 2007; Forget et al., 2006; Montmessin et al., 2007).”
Origin and evolution of a cold-based tropical mountain glacier on Mars: The Pavonis Mons fan-shaped deposit (2005, background): “[10] We have reexamined the Tharsis Montes fan-shaped deposits using new Mars Global Surveyor and Mars Odyssey data in conjunction with the previous Viking Orbiter data.”
Recent formation and evolution of northern Martian polar layered deposits as inferred from a Global Climate Model (2007, background): “They predict that during periods of high obliquity, polar surface ice could be unstable and transported to hightopography equatorial areas where many geological features indicate traces of remnant glaciers [Richardson and Wilson, 2002; Mischna et al., 2003a; Levrard et al., 2004; Forget et al., 20”
Hydration state of the Martian surface as seen by Mars Express OMEGA: 2. H2O content of the surface (2007, background): “Atmospheric and icestability models also predict that the exchange of water vapor between these two reservoirs has played an important role in the recent history of Mars [Forget et al., 2006; Mellon et al., 2004; Mischna et al., 2003; Mellon and Jakosky, 1995], though direct quantitative measureme”