A Boundary-Layer Model for Mars: Comparison with Viking Lander and Entry Data

Haberle, R. M.; Houben, H.; Hertenstein, Rolf; Herdtle, T.

doi:10.1175/1520-0469(1993)050<1544:ablmfm>2.0.co;2

Cited by 125 publications

(123 citation statements)

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“…This is likely due to the different phasing of the tides relative to the background circulation and the stronger Coriolis effect at the higher latitude of VL2 (e.g. Haberle et al 1993b). The wind turns clockwise through a full 360°in some seasons (L s ∼ 345°and 105°, Figs.…”

Section: Near-surface Wind Speed and Directionmentioning

confidence: 99%

The Modern Near-Surface Martian Climate: A Review of In-situ Meteorological Data from Viking to Curiosity

et al. 2017

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We analyze the complete set of in-situ meteorological data obtained from the Viking landers in the 1970s to today's Curiosity rover to review our understanding of the modern near-surface climate of Mars, with focus on the dust, CO 2 and H 2 O cycles and their impact on the radiative and thermodynamic conditions near the surface. In particular, we provide values of the highest confidence possible for atmospheric opacity, atmospheric pressure, near-surface air temperature, ground temperature, near-surface wind speed and direction, and near-surface air relative humidity and water vapor content. Then, we study the diurnal, seasonal and interannual variability of these quantities over a span of more thanThe original version of this article was revised because due to an unfortunate turn of events a wrong value was published in Table 1. The resolution of the PHX pressure sensor was published as "0.1 mbar" whereas this value has now been corrected to "0.1 Pa" which is the correct value and should be regarded as the final version by the reader. B G.M. Martínez

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Section: Near-surface Wind Speed and Directionmentioning

confidence: 99%

The Modern Near-Surface Martian Climate: A Review of In-situ Meteorological Data from Viking to Curiosity

et al. 2017

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“…In the convective late-morning boundary layer at 1000 LT the turbulent heating rate is strongly positive (more than C4 K h ¡1 ) and dominating from 100 m to 1500 m. Weaker convective heating extends up to 7000 m in the late afternoon. However, near the surface, the daytime radiative heating is so intense that turbulence is actually cooling the layers below 100 m despite the fact that these layers are very unstable, a peculiarity of the thin Martian atmosphere discussed, for example, by Savijärvi (1991b) and Haberle et al (1993). The activated convection is able to heat the air directly above the surface only shortly after sunrise (note the 0600 LT curve in Fig.…”

Section: (B) Radiation Considerationsmentioning

confidence: 92%

Mars pathfinder: New data and new model simulations

Savijärvi

Määttänen

Kauhanen

et al. 2004

Quart J Royal Meteoro Soc

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SUMMARYThe diurnal cycle in the temperature and wind speed of the Mars Path nder lander (MPF) is compared with the results from a one-dimensional high-solution boundary-layer model. The radiation scheme of the model has been validated against line-by-line calculations in an average Martian case. The agreement with MPF observations is good. Strong daytime turbulent variability and steep vertical temperature gradients characterize the observations. A detailed look at the model physics reveals that the thin atmosphere responds strongly to thermal radiation. During the daytime, absorption of surface-emitted thermal radiation by CO 2 , water vapour and dust is the main heating agent below 200 m despite the fact that the surface layer is strongly convective and dust absorbs solar radiation. The night-time inversion is also transferred to the air mainly by long-wave processes, although turbulent cooling dominates very near the surface (below 40 m). The near-surface net heating/cooling displays a sensitive balance between several large and opposite physical processes, wherefore accurate algorithms and high resolution are needed for detailed model results. The modelled hydrologic cycle reveals a well-mixed layer of up to 5 km with thin icy fog and frost forming in the night-time. These sublimate back to the air soon after sunrise.

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“…The results for uniform, moderately confined (to 10 km), and shallowly confined (to 6 km) dust distributions are shown in Plates lc and lf. We did not consider dust distributions shallower than 6 km since at the low and mid-latitude landing sites, the daytime boundary layer depth should in general be roughly 6 km [Haberle et al, 1993]. This effect of dust distribution assumption on the retrieval rams out to be rather small.…”

Section: Changes In the Vertical Distribution Of Dustmentioning

confidence: 99%

Seasonal variation of aerosols in the Martian atmosphere

Toigo¹,

Richardson²

2000

J. Geophys. Res.

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Abstract. Reanalysis of Viking Lander (VL) visible and VikingOrbiter infrared optical depth measurements shows that the visible to infrared ratio of total extinction opacity varies with season. The ratio is near to its previously reported constant value, 2.5, during dust storm periods and higher during northern spring and summer. The increase in ratio is hypothesized to be due to seasonally varying water ice haze, which produces a higher optical depth in the visible than in the infrared. This differs significantly from previous analyses of VL visible opacities which have assumed that only dust contributes to the optical depth measured during the early afternoon. Consequently we suggest that the Martian atmosphere is clearer of dust, especially during northern spring and summer, than previously suggested based upon VL data. We find dust visible optical depths of 0.1-0.4 during the northern spring and summer seasons, compared to previous estimates of 0.4-0.6. We also find that water ice hazes can provide roughly 50% of the total visible opacity in these seasons. For southern spring and summer, dust optical depths are more variable, but generally _>_0.4, with water ice opacity <0.1. The data suggest water ice optical depths are slightly higher and peak earlier (L,-80ø-90 ø) at VL1 than at VL2 (L,= 115 ø-130ø). We estimate average northern summer water (daytime minimum) ice masses to be roughly 0•1 -0.5 precipitable microns, depending on the assumed particle size distribution and hence 1 --5% of the total water column. The observation of significant and previously unrecognized amounts of water ice haze suggests a larger role for water in controlling atmospheric heating rates and the vertical distribution of dust and water vapor than has been widely accepted to date.

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A Boundary-Layer Model for Mars: Comparison with Viking Lander and Entry Data

Cited by 125 publications

References 0 publications

The Modern Near-Surface Martian Climate: A Review of In-situ Meteorological Data from Viking to Curiosity

The Modern Near-Surface Martian Climate: A Review of In-situ Meteorological Data from Viking to Curiosity

Mars pathfinder: New data and new model simulations

Seasonal variation of aerosols in the Martian atmosphere

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