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The results of the MAOAM modeling. The different columns show the modeling results under different assumption (see the text). Panel A shows the precipitated water vapor in μm; B shows the precipitated atmospheric ice in opacity units; and C shows the surface water ice in mm. The horizontal axis in all the panels plots the season in Ls; the vertical axis plots the latitude.
Source publication
Within the numerical general-circulation model of the Martian atmosphere MAOAM (Martian Atmosphere: Observation and Modeling), we have developed the water cycle block, which is an essential component of modern general circulation models of the Martian atmosphere. The MAOAM model has a spectral dynamic core and successfully predicts the temperature...
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Phase transitions of water molecules are commonly expected to occur only under extreme conditions, such as nanoconfinement, high pressure, or low temperature. We herein report the disordered-ordered phase transition of two-dimensional interfacial water molecules under ambient conditions using molecular-dynamics simulations. This phase transition is...
Citations
... Through the use of numerical models we are able to characterise Mars with limited observational data, allowing us to simulate areas where observational data are limited (Read et al., 2015;Martínez et al., 2017). Through these efforts our understanding of many atmospheric processes has been refined, including the annual CO 2 cycle (Forget et al., 1998;Malin et al., 2001;Aharonson et al., 2004;Hayne et al., 2012;Holmes et al., 2018;Banfield et al., 2020), CO 2 availability in the interest of terraforming (Jakosky and Edwards, 2018), its hydrological cycle (Houben et al., 1997;Haberle et al., 2001;Brown et al., 2014;Shaposhnikov et al., 2016Shaposhnikov et al., , 2018Singh et al., 2018;Pál et al., 2019), its surface topography (Smith et al., 1999;Richardson and Wilson, 2002;Zalucha et al., 2010) and the effects of the climatically dominant dust cycle (Kahre and Haberle, 2010;Wang and Richardson, 2015;Wang et al., 2018;Gebhardt et al., 2020;Ball et al., 2021;Chaffin et al., 2021). Simulations have been performed ranging in scale from global (Navarro et al., 2014;Streeter et al., 2020;Kass et al., 2020) to mesoscale levels (Montabone et al., 2006;Spiga and Forget, 2009;Newman et al., 2021). ...
... The Martian atmosphere features small amounts of water vapour which are generally increased during the colder aphelion months (Nazari-Sharabian et al., 2020). This humidity affects the radiative transfer in every layer through water vapour molecules and cloud condensate (Shaposhnikov et al., 2016;Steele et al., 2017;Shaposhnikov et al., 2018;Fischer et al., 2019). Mars has water ice clouds which influence radiative transfer between the surface and the upper atmosphere (e.g. ...
We present results from the Met Office Unified Model (UM), a world-leading climate and weather model, adapted to simulate a dry Martian climate. We detail the adaptation of the basic parameterisations and analyse results from two simulations, one with radiatively active mineral dust and one with radiatively inactive dust. These simulations demonstrate how the radiative effects of dust act to accelerate the winds and create a mid-altitude isothermal layer during the dusty season. We validate our model through comparison with an established Mars model, the Laboratoire de Météorologie Dynamique planetary climate model (PCM), finding good agreement in the seasonal wind and temperature profiles but with discrepancies in the predicted dust mass mixing ratio and conditions at the poles. This study validates the use of the UM for a Martian atmosphere, highlights how the adaptation of an Earth general circulation model (GCM) can be beneficial for existing Mars GCMs and provides insight into the next steps in our development of a new Mars climate model.
... The hydrological block of the model has been described in detail in previous articles (Shaposhnikov et al., 2016(Shaposhnikov et al., , 2018(Shaposhnikov et al., , 2019. The block includes a semi-Lagrangian scheme for the transfer of passive impurities, as well as the microphysics of water vapor and ice. ...
... The water cycle of the model includes a semi-Lagrangian transport of water vapor and ice (Shaposhnikov et al., 2016) and accounts for the microphysics of conversions between vapor and ice (Shaposhnikov et al., 2018). Condensation occurs on cloud condensation nuclei, whose sizes are represented by four characteristic bins. ...
Plain Language Summary
Transport of water to the Martian upper atmosphere with subsequent photodissociation and escape of hydrogen into space occurs near perihelion and amplifies during global dust storms. One explanation is the so‐called water “pump” due to the seasonally varying global meridional circulation. Forcing by atmospheric gravity waves (GWs) is a major mechanism that drives this circulation in the middle and upper atmosphere. The interplay between GWs, dust storms and transport of water from the lower atmosphere to the thermosphere has been explored with a Martian general circulation model. When dust storms take place at equinoxes, GWs enhance warming in polar regions and accumulation of vapor there. They also strengthen the uplift in low latitudes leading to a significant increase of water in the thermosphere. When global dust storms start to decay, wave forcing helps to remove water from upper layers of the atmosphere more abruptly. When storms onset near the perihelion solstice (southern hemisphere summer), GWs delay the upward transport of water over the south pole first, but then intensify it and the redistribution across the globe. Thus, more water is delivered to the thermosphere during dust storms and, potentially, can escape to space as atomic hydrogen.
... The subgrid-scale GW spectral parameterization was described in the work of Medvedev et al. (2011), and its recent application to studying global effects of GWs is given in the work by Yigit et al. (2018). Other model parameters are the same as in the study of Medvedev et al. (2016). ...
... The water cycle of the model includes a semi-Lagrangian transport of water vapor and ice (Shaposhnikov et al., 2016) and accounts for the microphysics of conversions between vapor and ice (Shaposhnikov et al., 2018). Condensation occurs on cloud condensation nuclei (CCN), whose sizes are represented by four characteristic bins. ...
Simulations with the Max Planck Institute Martian general circulation model for Martian years 28 and 34 reveal details of the water "pump" mechanism and the role of gravity wave (GW) forcing. Water is advected to the upper atmosphere mainly by upward branches of the meridional circulation: in low latitudes during equinoxes and over the south pole during solstices. Molecular diffusion plays little role in water transport in the middle atmosphere and across the mesopause. GWs modulate the circulation and temperature during global dust storms, thus changing the timing and intensity of the transport. At equinoxes, they facilitate water accumulation in the polar warming regions in the middle atmosphere followed by stronger upwelling over the equator. As equinoctial storms decay, GWs tend to accelerate the reduction of water in the thermosphere. GWs delay the onset of the transport during solstitial storms and change the globally averaged amount of water in the upper atmosphere by 10-25%.
... Dans les années 2000, un modèle japonais Kuroda et al., 2013) et un modèle européen en Allemagne (Hartogh et al., 2005;Bell et al., 2007;McDunn et al., 2010;Shaposhnikov et al., 2016) voient le jour. Ces deux modèles se sont associés, partageant une physique commune, et ont notamment servi à étudier l'effet global des ondes de gravité sur l'atmosphère (Medvedev et al., 2011Yigit et al., 2015;Kuroda et al., 2015Kuroda et al., , 2019. ...
Cette thèse porte sur l'amélioration de la représentation de l'atmosphère de la planète Mars par le Modèle de Climat Global (« GCM ») martien du Laboratoire de Météorologie Dynamique (LMD). Le GCM martien développé au LMD en collaboration avec plusieurs équipes européennes (LATMOS, IAA Grenade, University of Oxford, The Open University), et avec le soutien de l'ESA et du CNES, est utilisé pour de nombreuses applications. Ce modèle s'efforce de prédire le comportement détaillé du climat martien décrit par les cycles du dioxyde de carbone, de l'eau, des poussières et de la photochimie, uniquement à partir d'équations universelles. La comparaison des simulations du GCM avec les observations disponibles permet de les interpréter, et révèle parfois que certains processus climatiques martiens restent mal modélisés. Le travail de cette thèse consiste à étudier et paramétriser l'effet de certains de ces mécanismes sous-maille, c'est-à-dire non résolus directement par le modèle. À l'aide de l'analyse et de la modélisation de ces processus on tente de corriger les défauts du modèle concernant la distribution verticale de la vapeur et de la glace d'eau, ainsi que les échanges avec la surface, la distribution verticale des poussières, avec notamment la modélisation des couches détachées de poussière, et bien sûr les effets de leurs couplages. Mais aussi, on s'intéresse aux phénomènes sous-maille de l'atmosphère qui peuvent avoir un impact extrêmement important sur la circulation globale, en particulier les ondes de gravité non-orographiques que j'ai étudiées en analysant les observations de la mission MAVEN.
... On the other hand, General Circulation Models (GCMs), usually without taking into account chemistry Barnes et al., 1993;Shaposhnikov et al., 2016) have been extended to include photochemistry and are now able to simulate such interactions (Lefevre et al., 2004;2008;Neary and Daerden, 2017;Moudden and McConnell, 2005;González-Galindo et al., 2005;Holmes et al., 2017;Holmes et al., 2018) due to advances in High Performance Computing (HPC). As compared to being constrained by an atmospheric vertical column (e.g., 1D models), GCMs model the entire atmosphere. ...
Odd oxygen (O, O(^1D), O_3) abundance and its variability in the Martian atmosphere results from complex physical and chemical interactions among atmospheric species, which are driven mainly by solar radiation and atmospheric conditions. Although our knowledge of Mars’ ozone distribution and variability has been significantly improved with the arrival of several recent orbiters, the data acquired by such missions is not enough to properly characterize its diurnal variation. Thus, photochemical models are useful tools to assist in such a characterization. Here, both the Martian ozone vertical distribution and its diurnal variation for equatorial latitudes are studied, using the JPL/Caltech one-dimensional photochemical model and diurnally-variable atmospheric profiles. The chosen equatorial latitude-region is based on the recent and future plans of NASA and other agencies to study this region by different surface missions. A production and loss analysis is performed in order to characterize the chemical mechanisms that drive odd oxygen's diurnal budget and variability on Mars making use of the comprehensive chemistry implemented in the model. The diurnal variation shows large differences in the abundance between daytime and nighttime; and variable behavior depending on the atmospheric layer. The photolysis-driven ozone diurnal profile is obtained at the surface, whilst a sharp decrease is obtained in the upper troposphere at daytime, which originates from the large differences in atomic oxygen abundances between atmospheric layers. Finally, no clear anticorrelation between ozone and water vapor is found in the diurnal cycle, contrary to the strong correlation observed by orbiters on a seasonal timescale.
... The hydrological part of the model has been described in detail in the papers of Shaposhnikov et al. (2016Shaposhnikov et al. ( , 2018a. It includes a semi-Lagrangian transport of water vapor and ice and accounts for the microphysics of vapor-ice conversions. ...
We present results of simulations with the Max Planck Institute Martian general circulation model implementing a hydrological cycle scheme. The simulations reveal a seasonal water “pump” mechanism responsible for the upward transport of water vapor. This mechanism occurs in high latitudes above 60° of the southern hemisphere at perihelion, when the upward branch of the meridional circulation is particularly strong. A combination of the mean vertical flux with variations induced by solar tides facilitates penetration of water across the “bottleneck” at approximately 60 km. The meridional circulation then transports water across the globe to the northern hemisphere. Since the intensity of the meridional cell is tightly controlled by airborne dust, the water abundance in the thermosphere strongly increases during dust storms.
... The hydrological part of the model has been described in detail in the papers of Shaposhnikov et al. [2016Shaposhnikov et al. [ , 2018a. It includes a semi-Lagrangian transport of water vapor and ice, and accounts for the microphysics of vapor-ice conversions. ...
We present results of simulations with the Max Planck Institute general circulation model (MPI-MGCM) implementing a hydrological cycle scheme. The simulations reveal a seasonal water "pump" mechanism responsible for the upward transport of water vapor. This mechanism occurs in high latitudes above 60 of the southern hemisphere at perihelion, when the upward branch of the meridional circulation is particularly strong. A combination of the mean vertical flux with variations induced by solar tides facilitates penetration of water across the "bottleneck" at approximately 60 km. The meridional circulation then transports water across the globe to the northern hemisphere. Since the intensity of the meridional cell is tightly controlled by airborne dust, the water abundance in the thermosphere strongly increases during dust storms.
... The most recent applications of this MGCM along with the current setup are presented in the works of Medvedev et al. [2013Medvedev et al. [ , 2015Medvedev et al. [ , 2016 and Yiğit et al. [2015]. The earlier version of the hydrological scheme has been described in the work of [Shaposhnikov et al., 2016]. ...
... Instead, we adopted the advection based on a semi-Lagrangian explicit monotone secondorder hybrid scheme and on the time splitting method in three spatial directions [Mingalev et al., 2010]. A thorough examination of performed runs has confirmed that this scheme maintains a high order of conservation of water masses and solution accuracy appropriate for general circulation modeling [Shaposhnikov et al., 2016]. In addition to advection, transport includes diffusion and mixing associated with subgrid-scale processes. ...
... The model runs have been initialized with the distribution of water vapor in the atmosphere obtained in our earlier experiments [Shaposhnikov et al., 2016]. As a reminder, the previous simulations started with a linear latitudinal gradient of water vapor (from 0 in the south to 200 ppm in the north) and no ice outside the caps was prescribed anywhere in the atmosphere at the beginning. ...
We present a new implementation of the hydrological cycle scheme into a general circulation model of the Martian atmosphere. The model includes a semi-Lagrangian transport scheme for water vapor and ice, and accounts for microphysics of phase transitions between them. The hydrological scheme includes processes of saturation, nucleation, particle growth, sublimation and sedimentation under the assumption of a variable size distribution. The scheme has been implemented into the Max Planck Institute Martian general circulation model (MPI--MGCM) and tested assuming mono- and bimodal log-normal distributions of ice condensation nuclei. We present a comparison of the simulated annual variations, horizontal and vertical distributions of water vapor and ice clouds with the available observations from instruments onboard Mars orbiters. The accounting for bi-modality of aerosol particle distribution improves the simulations of the annual hydrological cycle, including predicted ice clouds mass, opacity, number density, particle radii. The increased number density and lower nucleation rates brings the simulated cloud opacities closer to observations. Simulations show a weak effect of the excess of small aerosol particles on the simulated water vapor distributions.
... The most recent applications of this MGCM along with the current setup are presented in the works of Medvedev et al. (2013Medvedev et al. ( , 2015Medvedev et al. ( , 2016 and Yigit et al. (2015). The earlier version of the hydrological scheme has been described in the work of Shaposhnikov et al. (2016). ...
... Instead, we adopted the advection based on a semi-Lagrangian explicit monotone second-order hybrid scheme and on the time splitting method in three spatial directions (Mingalev et al., 2010). A thorough examination of performed runs has confirmed that this scheme maintains a high order of conservation of water masses and solution accuracy appropriate for general circulation modeling (Shaposhnikov et al., 2016). In addition to advection, transport includes diffusion and mixing associated with subgrid-scale processes. ...
... The model runs have been initialized with the distribution of water vapor in the atmosphere obtained in our earlier experiments (Shaposhnikov et al., 2016). As a reminder, the previous simulations started with a linear latitudinal gradient of water vapor (from 0 in the south to 200 ppm in the north) and no ice outside the caps was prescribed anywhere in the atmosphere at the beginning. ...
We present a new implementation of the hydrological cycle scheme into a general circulation model of the Martian atmosphere. The model includes a semi-Lagrangian transport scheme for water vapor and ice and accounts for microphysics of phase transitions between them. The hydrological scheme includes processes of saturation, nucleation, particle growth, sublimation, and sedimentation under the assumption of a variable size distribution. The scheme has been implemented into the Max Planck Institute Martian general circulation model and tested assuming monomodal and bimodal lognormal distributions of ice condensation nuclei. We present a comparison of the simulated annual variations, horizontal and vertical distributions of water vapor, and ice clouds with the available observations from instruments on board Mars orbiters. The accounting for bimodality of aerosol particle distribution improves the simulations of the annual hydrological cycle, including predicted ice clouds mass, opacity, number density, and particle radii. The increased number density and lower nucleation rates bring the simulated cloud opacities closer to observations. Simulations show a weak effect of the excess of small aerosol particles on the simulated water vapor distributions.
