A study of the thermal and dynamical structure of the martian lower atmosphere

Gierasch, P. J.; Goody, R. M.

doi:10.1016/0032-0633(68)90102-5

Cited by 238 publications

(113 citation statements)

References 15 publications

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“…Vertical turbulent heat transport is supposed to be very small, because the observed vertical temperature profiles indicate very stable features in Mariner 6, 7 and 9 observations. If the atmosphere is stably stratified, turbulence is strongly suppressed and has associated value of the vertical eddy diffusivity less than the effective radiative diffusivity (Gierasch and Goody, 1968) Consequently, the effect due to turbulence would be negligible, compared with the fact that dust has very large contribution to the thermal condition of the Martian atmosphere as shown above.…”

Section: Basic Equations For Radiative Transfermentioning

confidence: 95%

“…(14) and (15), we used the same method of an iterative numerical integration as Yamamoto et al (1974). If I(*, -*) and I(*, *) are obtained, the downward and upward fluxes of the diffuse radiation field at any given level can be readily written as Gierasch and Goody (1973).…”

Section: Basic Equations For Radiative Transfermentioning

confidence: 99%

“…Not only great dust storms but also strong slope winds or dust devils, which frequently occur on the Mars, would supply dust into the atmosphere unceasingly (Gierasch and Goody, 1973;Blumsack et al, 1973;Leovy et al, 1973). However, most of studies on the Martian atmospheric phenomena have been carried out on the basis of assumption of dust-free atmosphere (e.g., Gierasch and Goody, 1968;Leovy and Mintz, 1969).…”

Section: Introductionmentioning

confidence: 99%

“…The thermal tide is likely to be strongly related with the thermal effects due to dust. Absorption of solar radiation due to dust is also a very important term as energy source of atmospheric motion (Gierasch and Goody, 1973;Golitsyn, 1973;Hess, 1973: Leovy et al, 1973 In the previous paper (Moriyama, 1974), we studied the effect of dust on infrared radiation transfer, and pointed out its importance to the thermal structure of the Martian atmosphere. As an extension of our study on radiative effects of dust, now we investigate quantitatively heating of the Martian atmosphere due to absorption of the visible solar radiation in the present paper.…”

Section: Introductionmentioning

confidence: 99%

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Effects of Dust on Radiation Transfer in the Martian Atmosphere (II)

Moriyama

1975

Journal of the Meteorological Society of Japan

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Section: Basic Equations For Radiative Transfermentioning

confidence: 95%

Section: Basic Equations For Radiative Transfermentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Effects of Dust on Radiation Transfer in the Martian Atmosphere (II)

Moriyama

1975

Journal of the Meteorological Society of Japan

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“…Cheap, simple one-dimensional models have been used to study specific processes that do not require full solution of the dynamic equations. Examples are the radiative transfer model by Gierasch and Goody (1968), regolith-atmosphere water exchange by Jakosky (1985) and water ice cloud formation by Michelangeli et al (1993). The Mars Climate Simulator is designed to close the gap between these simple models and the fully complex GCMs to investigate mainly the paleo climate of Mars.…”

Section: Introductionmentioning

confidence: 99%

Response of the intermediate complexity Mars Climate Simulator to different obliquity angles

Segschneider

Grieger

Keller

et al. 2005

Planetary and Space Science

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A climate model of intermediate complexity, named the Mars Climate Simulator, has been developed based on the Portable University Model of the Atmosphere (PUMA). The main goal of this new development is to simulate the climate variations on Mars resulting from the changes in orbital parameters and their impact on the layered polar terrains (also known as permanent polar ice caps). As a first step towards transient simulations over several obliquity cycles, the model is applied to simulate the dynamical and thermodynamical response of the Martian climate system to different but fixed obliquity angles. The model is forced by the annual and daily cycle of solar insolation. Experiments have been performed for obliquities of φ = 15 • (minimum), φ = 25.2 • (present), and φ = 35 • (maximum). The resulting changes in solar insolation mainly in the polar regions impact strongly on the cross-equatorial circulation which is driven by the meridional temperature gradient and steered by the Martian topography. At high obliquity, the cross-equatorial near surface flow from the winter to the summer hemisphere is strongly enhanced compared to low obliquity periods. The summer ground temperature ranges from 200 K (φ = 15 • ) to 250 K (φ = 35 • ) at 80 • N in northern summer, and from 220 K (φ = 15 • ) to 270 K (φ = 35 • ) at 80 • S in southern summer. In the atmosphere at 1 km above ground, the respective range is 195-225 K in northern summer, and 210-250 K in southern summer.

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Large Eddy Simulations of the Dusty Martian Convective Boundary Layer with MarsWRF

Richardson

Zhang

et al. 2020

Preprint

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Large eddy simulation (LES) of the Martian convective boundary layer (CBL) with a Mars-adapted version of the Weather Research and Forecasting model (MarsWRF) is used to examine aerosol dust radiative-dynamical feedback upon turbulent mixing. The LES is validated against spacecraft observations and prior modeling. To study dust redistribution by coherent dynamical structures within the CBL, two radiatively-active dust distribution scenarios are used-one in which the dust distribution remains fixed and another in which dust is freely transported by CBL motions. In the fixed dust scenario, increasing atmospheric dust loading shades the surface from sunlight and weakens convection. However, a competing effect emerges in the free dust scenario, resulting from the lateral concentration of dust in updrafts. The resulting enhancement of dust radiative heating in upwelling plumes both generates horizontal thermal contrasts in the CBL and also increases buoyancy production, jointly enhancing CBL convection. We define a dust inhomogeneity index (DII) to quantify how much dust is concentrated in upwelling plumes. If the DII is large enough, the destabilizing effect of lateral heating contrasts can exceed the stabilizing effect of surface shading such that the CBL depth increases with increasing dust optical depth. Thus, under certain combinations of total dust optical depth and the lateral inhomogeneity of dust, a positive feedback may exist among dust optical depth, the vigor and depth of CBL mixing, and-to the extent that dust lifting is controlled by the depth and vigor of CBL mixing-the further lifting of dust from the surface.

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A study of the thermal and dynamical structure of the martian lower atmosphere

Cited by 238 publications

References 15 publications

Effects of Dust on Radiation Transfer in the Martian Atmosphere (II)

Effects of Dust on Radiation Transfer in the Martian Atmosphere (II)

Response of the intermediate complexity Mars Climate Simulator to different obliquity angles

Large Eddy Simulations of the Dusty Martian Convective Boundary Layer with MarsWRF

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