Weather and climate on Mars

Leovy, Conway Β.

doi:10.1038/35084192

Cited by 150 publications

(82 citation statements)

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“…For the Martian atmosphere, which is predominantly CO 2 [Leovy, 2001], we have c = 240 K and m 0 = 1.48 × 10 −5 kg/m s at T 0 = 293.15 K [ Crane Company, 1988].…”

Section: Analytical Model Of the Impact Thresholdmentioning

confidence: 99%

“…Although the numerical study of Kok [2010] quantified the impact threshold for a particular surface pressure and temperature, the high computational cost makes this method difficult to use in determining the impact threshold for the wide range of thermodynamic conditions occurring on Mars [Leovy, 2001]. Here, I therefore develop an analytical model capable of calculating the impact threshold for a wide range of thermodynamic conditions.…”

Section: Introductionmentioning

confidence: 99%

“…[2] Saltation, the wind-driven hopping motion of sand grains, forms dunes and ripples [Bagnold, 1941], and ejects fine dust into the atmosphere of Mars, which greatly affects its climate [Leovy, 2001]. Moreover, electric fields generated in saltation and dust storms [Kok and Renno, 2008] could affect atmospheric chemistry [Kok and Renno, 2009a] and produce electric discharges [Ruf et al, 2009].…”

Section: Introductionmentioning

confidence: 99%

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An improved parameterization of wind‐blown sand flux on Mars that includes the effect of hysteresis

Kok

2010

Geophysical Research Letters

113

210

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[1] Saltation, the wind-driven hopping motion of sand grains, forms dunes and ripples, and ejects fine dust particles into the atmosphere on Mars. Although the wind speed at which saltation is initiated, the "fluid threshold," has been studied extensively, the wind speed at which saltation is halted, the "impact threshold," has been poorly quantified for Mars conditions. I present an analytical model of the impact threshold, which is in agreement with measurements and numerical simulations for Earth conditions. For Mars conditions, the impact threshold is approximately an order of magnitude below the fluid threshold, in agreement with previous studies. Saltation on Mars can thus be sustained at wind speeds an order of magnitude less than required to initiate it, leading to the occurrence of hysteresis. I include the effect of hysteresis into an improved parameterization of sand transport on Mars.

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“…For the Martian atmosphere, which is predominantly CO 2 [Leovy, 2001], we have c = 240 K and m 0 = 1.48 × 10 −5 kg/m s at T 0 = 293.15 K [ Crane Company, 1988].…”

Section: Analytical Model Of the Impact Thresholdmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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An improved parameterization of wind‐blown sand flux on Mars that includes the effect of hysteresis

Kok

2010

Geophysical Research Letters

113

210

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“…3 GCM Wang and Ingersoll, 2003 eccentricity Greeley et al, 1993;Forget et al, 1999;Newman et al, 2002;Figs. 2, 3 Thomas et al, 1984;Greeley et al, 1993 Zurek andMartin, 1993;Cantor et al, 2001;Leovy, 2001Cantor et al, 2001100 2 1999, 2001Cantor et al, 2001Leovy, 2001Cantor et al 2001MGS-MOC 1999 60° 80° 30° 60° 30° 60° 60° 80° Cantor et al, 2001 e.g., Thomas et al, 1984;Greeley et al, 1993 GCM Fig. 3 (Greeley et al, 1993).…”

mentioning

confidence: 99%

“…1 Greeley et al, 1993;Sullivan et al, 2005Greeley et al, 1994WilGreeley et al, 1994;WilGreeley et al, 1994;Williams andGreeley, 1994 Lorenz et al, 2006;Lorenz and Radebaugh, 2009 総説 Mariner 9 Viking 1970 e.g., Cutts and Smith, 1973;Thomas, 1982;Ward et al, 1985;Greeley et al, 1993;Anderson et al, 1999Anderson et al, 2001 Mars Global Surveyor MGS MGS-MOC 2006 Mars Reconnaissance Orbiter MRO Hi-RISE 1 25 cm e.g., Fenton et al, 2005;Hayward et al, 2007;Greeley et al, 2008;Hobbs et al, 2010;Silvestro et al, 2010;Chojnacki et al, 2011 2004 Mars Exploration Rovers MER Grotzinger et al, 2005;Metz et al, 2009;Squyres et al, 2009;Hayes et al, 2011 GCM Table 1 e.g., Leovy, 2001 e.g., Wang and Ingersoll, 2003 GCM; e.g., Greeley et al, 1993;Heberle et al, 1993;Forget et al, 1999;Heberle et al, 1999;Newman et al, 2002 2001 MGS MGS-TES Leovy, 2001;Smith et al, 2001 MGS-TES GCM GCM Greeley et al, 1993;Heberle et al, 1993;Forget et al, 1999;Newman et al, 2002;Figs. 2, 3 GCM 30° 30° 30° 30° Fig. 2 ...…”

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confidence: 99%

風成砂丘から見る火星およびタイタンの大気循環システム

Hasegawa¹

2012

Jour. Geol. Soc. Japan

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Eolian dunes are particularly suited for comprehensive planetary studies because they are generally present on terrestrial planets, including Earth, Mars, Venus, and Saturn s moon Titan. Although the distribution and orientation of eolian dunes are thought to record surface wind patterns and atmospheric circulation systems on planets and moons, the validity of this idea has not been fully tested. In this study, I compared general circulation model (GCM) reconstruc-I compared general circulation model (GCM) reconstruccompared general circulation model (GCM) reconstructions of the present-day atmospheric circulation systems on Mars and Titan with eolian dune orientations and dune field distributions. The reconstructed Martian surface wind patterns indicated by dune centroid azimuths (DCA) and dune slipface orientations (SF) are generally consistent with the predominant surface wind patterns during the northern Martian hemisphere winter. In addition, dune fields are concentrated in high-latitude areas adjacent to areas with strong winds associated with the descending part of the Hadley circulation cell. This indicates that the distribution of dune fields and dune orientation patterns provide a record of atmospheric circulation patterns on Mars. In comparison, dune orientation-based wind pattern reconstructions on Titan are not consistent with GCM-based atmospheric circulation patterns. This discrepancy is thought to relate to occasional fast westerly winds during equinoxes that dominate the eastward streamlining pattern of Titan s dunes. Nevertheless, dune field distributions are reflected in atmospheric circulation patterns on Titan. Therefore, although eolian dune orientations are not always consistent with prevailing planetary and lunar atmospheric circulation patterns, the distribution of dune fields generally does reflect these patterns.

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On Mars too expect macroweather

Lovejoy

Müller²,

Boisvert

2014

Geophysical Research Letters

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Terrestrial atmospheric and oceanic spectra show drastic transitions at τ w ≈ 10 days and τ ow ≈ 1 year, respectively; this has been theorized as the lifetime of planetary-scale structures. For wind and temperature, the forms of the low-and high-frequency parts of the spectra (macroweather and weather) as well as the τ w can be theoretically estimated, the latter depending notably on the solar-induced turbulent energy flux. We extend the theory to other planets and test it using Viking lander and reanalysis data from Mars. When the Martian spectra are scaled by the theoretical amount, they agree very well with their terrestrial atmospheric counterparts. We discuss the implications for understanding planetary fluid dynamical systems.

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Weather and climate on Mars

Cited by 150 publications

References 46 publications

An improved parameterization of wind‐blown sand flux on Mars that includes the effect of hysteresis

An improved parameterization of wind‐blown sand flux on Mars that includes the effect of hysteresis

風成砂丘から見る火星およびタイタンの大気循環システム

On Mars too expect macroweather

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