Long term evolution and chaotic diffusion of the insolation quantities of Mars

By Jacques Laskar, A. Correia, Mickaël Gastineau, F. Joutel, B. Levrard, P. Robutel. 2004

955 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Molecular Biology

View Paper: https://www.semanticscholar.org/paper/b40b4badbec479f04c361de3b5e7d5263760bceb

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Citations in the corpus

North polar cap of Mars: Polar layered deposit characterization and identification of a fundamental climate signal (2005, positive): “[39] Climatemodels[e.g.,Jakoskyetal.,1995;Richardson and Wilson, 2002;Haberle et al., 2003; Mischna et al., 2003] using calculated orbital variations [e.g., Touma and Wisdom, 1993; Laskar and Robutel, 1993; Laskar et al., 2004 ] have examined how the regions of water ice stability change with Marti”
Cyclostratigraphy and its revolutionizing applications in the earth and planetary sciences (2013, methodology): “…(Huang et al., 2010a), and the Late Permian Wujiaping-Dalong Formations have a 34 k.y. obliquity cycle (Wu et al., 2013), which indicate 23 h and 22 h days, respectively, and which are consistent with the tidal dissipation model adopted for the La2004 astronomical solution (Laskar et al., 2004a).”
Impact crater formation in icy layered terrains on Mars (2006, background): “…significant variations in global climate, including the possibility of a warmer, wetter early period (e.g., Fanale et al. 1992; Owen 1992; Phillips et al. 2001; Poulet et al. 2005 Bibring et al. 2006) and recent rapid climate excursions resulting from obliquity changes (e.g., Laskar et al. 2004).”
Transverse Aeolian Ridges (TARs) on Mars (2008, background): “Themantle is geologically very recent and is thought to be deposited and removed cyclically as a result of episodic climate change driven by orbital dynamics, in particular variations in the obliquity of Mars rotation (Laskar et al., 2004).”
Rapid stepwise onset of Antarctic glaciation and deeper calcite compensation in the Pacific Ocean (2005, methodology): “We have developed a new chronology for these sections, based on detailed correlation of geological data to astronomically calculated variations of Earth's orbit and solar insolation (ref”
3D modelling of the early Martian Climate under a denser CO2 atmosphere: Temperatures and CO2 ice clouds. (2012, methodology): “8 (the most likely obliquity for Mars according to Laskar et al. (2004)).”
Amazonian northern mid-latitude glaciation on Mars: A proposed climate scenario (2009, methodology): “For example, using the orbital calculations of Laskar et al. (2004) and the LMD/GCM (Forget et al., 1999), Levrard et al. (2004) came to the conclusion that the tropical mountain glaciers and the latitude-dependent mantle can be formed during periods of high (35–40°) and low (15–25°) mean obliquity…”
Geologic history of Mars (2010, background): “During the current epoch the obliquity oscillates between 15° and 35° about a mean of 24°, but Laskar et al. (2004) estimate that the average obliquity over geologic time is 40° and that there is a 63% probability that the obliquity reached 60° in the last 1 Gyr.”
The current martian cratering rate (2010, background): “05 (e.g. Armstrong et al., 2004; Laskar et al., 2004) (known because of the chaotic nature of the variation).”
Recent formation and evolution of northern Martian polar layered deposits as inferred from a Global Climate Model (2007, methodology): “This last period becomes dominant when the variations of the obliquity are minimal [see also Laskar et al., 2002, 2004 ].”
Tropical mountain glaciers on Mars: Altitude-dependence of ice accumulation, accumulation conditions, formation times, glacier dynamics, and implications for planetary spin-axis/orbital history (2007, methodology): “Climate change on Mars is controlled by spin-axis and orbital variations similar to those thought to cause ice ages on Earth (Imbrie, 1982, 1985; Laskar et al., 2004).”
The Climate of Early Mars (2016, background): “Mars’ orbital eccentricity and obliquity evolve chaotically on long timescales, however, and have probably varied over ranges of 0 – 0.125 and 10◦ – 60◦, respectively (Laskar et al. 2004).”