Southern Martian winter weather associated with baroclinic topography forced Rossby waves: analysing by Global Mars Multiscale Model

Fazel-Rastgar, Farahnaz

doi:10.1007/s10509-019-3541-0

Cited by 2 publications

(2 citation statements)

References 22 publications

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“…Hence, in many sites, these flows greatly affect processes such as the surface pressure diurnal cycle (Tyler Jr et al., 2002), near‐surface winds, aeolian activity, etc. For example, this occurs in Arsia Mons (Savijärvi & Siili, 1993), Hellas basin (Fazel‐Rastgar, 2019; Newman et al., 2002a, 2002b), Argyre basin (Fazel‐Rastgar, 2019), Hellespontus Montes, Hellas and Isidis Planitia (Chojnacki et al., 2019), Chryse and Utopia Planitia, landing sites of the Viking lander 1 and 2 (VL1 and VL2), respectively (Haberle et al., 1993), Valles Marineris, landing site of the Mars Pathfinder (MPF) rover (Tyler Jr et al., 2002), Aeolis Mons in Gale Crater, landing site of the Mars Science Laboratory (MSL)/Curiosity rover (Baker et al., 2018; Kite et al., 2013; Newman et al., 2017; Pla‐García et al., 2016; Rafkin et al., 2016; Richardson & Newman, 2018; Soria‐Salinas et al., 2020), and Jezero Crater, landing site of the Mars 2020 Perseverance rover (Pla‐García et al., 2020; Viúdez‐Moreiras, de la Torre, et al., 2022; Viúdez‐Moreiras, Lemmon, et al., 2022). The magnitude and timing of the winds predicted (Newman et al., 2021) and measured (Newman et al., 2022; Viúdez‐Moreiras, Lemmon, et al., 2022) in Jezero are reported to be consistent with primary control by regional and local slope flows.…”

Section: State Of the Artmentioning

confidence: 99%

“…Table 1 also shows that modeling approaches to the Earth's atmosphere such as the NASA Ames global circulation model (GCM), the fifth‐Generation Penn State University/National Center for Atmospheric Research (NCAR) Mesoscale Model (MM5), and the Weather Research and Forecasting (WRF) model have been adapted to studies on Mars, as the so‐called MGCM (Newman et al., 2002a, 2002b; Savijäarvi, 1999; Tyler et al., 2002), MMM5 (Tyler et al., 2002), and MarsWRF (Baker et al., 2018; Newman et al., 2017; Newman et al., 2022; Pla‐García et al., 2020; Vicente‐Retortillo et al., 2018; Viúdez‐Moreiras, Lemmon, et al., 2022; Zhao et al., 2021), respectively. Other models in the literature are the Global Mars Multiscale Model (GM3) (Fazel‐Rastgar, 2019; Moudden & McConnell, 2005), Mars Global Reference Atmospheric Model (Mars‐GRAM) (Justus et al., 2006), and Mars Regional Atmospheric Modeling System (MRAMS) (Love et al., 2022; Pla‐García et al., 2016, 2020; Rafkin et al., 2016). Moreover, wind measurements at both VL1 and VL2 landing sites, which exhibit a diurnal cycle that is mainly due to slope winds, were recreated through mesoscale modeling (Haberle et al., 1993), and Martian PBL phenomena were studied using Prandtl's theory, a 2D mesoscale model, and VL1 data (Savijärvi & Siili, 1993).…”

Section: State Of the Artmentioning

confidence: 99%

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Thermally Driven Winds on Mars: A Review and a Slope Effect Numerical Study

Montlaur,

Arias,

Rojas

2024

JGR Planets

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Regional and local thermally driven winds are planetary boundary layer phenomena frequently observed on Mars over sloping and flat regions, when diurnal surface temperature variations are significant and large‐scale winds are sufficiently weak. In particular, slope flows are prevalent in many areas on Mars, where they can reach high speeds and have a substantial impact on the near‐surface wind patterns, pressure diurnal cycle, aeolian activity, etc. This work first reviews literature on Martian winds, listing wind speeds obtained either numerically or from in situ measurements, with special emphasis on slope flows. Second, a methodology is presented to perform numerical simulations of slope flows on Mars using the open‐source computational fluid dynamics code OpenFOAM. Slope winds are then studied in a simplified Martian mountain‐valley configuration, using realistic values for various parameters, such as the slope angle and temperature variation. The incompressible Navier‐Stokes equations with Boussinesq approximation are used, along with the k‐ɛ Reynolds‐averaged Navier‐Stokes turbulence model. Radiant heat transfer is included and proven to be paramount for a correct description of Martian slope winds. Results of velocity and temperature profiles are obtained for various slope angles. These simulations aim to provide further insight on the behavior of slope winds on Mars, to simplify the process of assessing numerous potential landing sites for upcoming missions, since these highly regular winds could be useful, for instance, for dust removal applications.

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Section: State Of the Artmentioning

confidence: 99%

Section: State Of the Artmentioning

confidence: 99%

Thermally Driven Winds on Mars: A Review and a Slope Effect Numerical Study

Montlaur,

Arias,

Rojas

2024

JGR Planets

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Observations of Gravity Waves in the Middle Atmosphere of Mars

Saunders¹,

Withers²

2021

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Gravity waves are ubiquitous throughout the atmosphere of Mars. Their propagation and dissipation influence the circulation and thermal structure of the middle and upper atmosphere. Yet there have been few studies of gravity wave characteristics in the middle atmosphere, a region that is critical for their propagation from generation in the lower atmosphere to dissipation and associated exchanges of momentum and energy in the upper atmosphere. There have been few studies because few atmospheric profiles span the middle atmosphere with the kilometer-scale or smaller vertical resolution that is Required to characterize gravity waves. Here we report the characterization of gravity waves in the middle atmosphere using 12 high-resolution atmospheric density profiles. Four of these were acquired from a ground-based stellar occultation from 1976 that yielded immersion and emersion profiles on opposite sides of the planet, and the remaining eight were measured during atmospheric entry by landers and rovers. Predominant wavelengths were 3–14 km, and amplitudes were generally 0.8%–2.5%. Where static stability is large and positive, gravity waves grow efficiently. In other instances, static stability is not large and positive over a wide altitude range, and gravity wave amplitudes do not behave as neatly. These observations of gravity waves in the middle atmosphere of Mars can be used to test gravity wave parameterizations in large-scale general circulation models and to investigate predictions for how gravity wave propagation and dissipation influence the circulation and thermal structure of the middle and upper atmosphere.

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Southern Martian winter weather associated with baroclinic topography forced Rossby waves: analysing by Global Mars Multiscale Model

Cited by 2 publications

References 22 publications

Thermally Driven Winds on Mars: A Review and a Slope Effect Numerical Study

Thermally Driven Winds on Mars: A Review and a Slope Effect Numerical Study

Observations of Gravity Waves in the Middle Atmosphere of Mars

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