Numerical simulation of the hydrological cycle of Mars / Численное моделирование гидрологического цикла Марса тема диссертации и автореферата по ВАК РФ 01.03.04, кандидат наук Шапошников Дмитрий Сергеевич

• Шапошников Дмитрий Сергеевич
• кандидат наук
• 2019

Оглавление диссертации кандидат наук Шапошников Дмитрий Сергеевич

Contents

Page

Introduction

Chapter 1. The planet Mars

1.1 General information

1.1.1 Orbital and physical parameters

1.1.2 Martian calendar

1.1.3 Topography

1.1.4 Evolution of Mars

1.2 Atmosphere and climate of Mars

1.3 Physics of water

1.4 Hydrological cycle

1.4.1 Historical view

1.4.2 Modern concepts

1.5 Discussion and conclusions

Chapter 2. General circulation model

2.1 Governing equations

2.2 Hydrological scheme

2.2.1 Tracer transport

2.2.2 Diffusion

2.2.3 Dust scenarios

2.2.4 Sedimentation

2.2.5 Bimodal distribution

2.2.6 Saturation

2.2.7 Nucleation

2.2.8 Particle growth

2.2.9 Interactions with surface

2.2.10 Photodissociation

2.3 Discussion and conclusions

Page

Chapter 3. Bimodal size distribution of dust

3.1 Design of simulations

3.2 Annual variations

3.3 Longitudinal variations

3.4 Vertical distribution

3.5 Monomodal dust distribution

3.5.1 Annual cycle

3.5.2 Time step dependency

3.5.3 Vertical profiles

3.5.4 Aphelion cloud belt

3.6 Discussion and conclusions

Chapter 4. Water "pump" mechanism

4.1 Design of simulations

4.2 Vertical transport

4.3 Transport at perihelion

4.4 Dust storm

4.5 Local time variations

4.6 Comparison with observations

4.7 Discussion and Conclusions

Summary and conclusions

Acknowledgements

Bibliography

Введение диссертации (часть автореферата) на тему «Numerical simulation of the hydrological cycle of Mars / Численное моделирование гидрологического цикла Марса»

Introduction

Studying the planets and small bodies of the Solar System is of paramount importance for understanding its origin and development. But above all, it provides the key to finding the likely paths of the future evolution of our planet and understanding how to keep Earth habitable for future generations.

Mars is the fourth planet from the Sun in the Solar System and the closest one to Earth among the other planets. At present, Mars is the most interesting and the most explored planet of the Solar System after Earth. The climate conditions on Mars, although being unsuitable for life, are the most similar to those on Earth. Presumably, in the past, the Martian climate could have been warmer and wetter; there was liquid water on its surface, and it even rained. Mars is the most likely destination for the first manned mission to another planet. However, the main thing is that Mars is so far the only planet that holds promise in terms of human development [1].

The Martian climate is mainly determined by the processes occurring in its atmosphere, such as the movement of air masses, convective mixing, radiative transfer, and transport of tracers. It is impossible to measure atmospheric fields, e.g. velocity, in full detail, neither on Earth, nor on other planets. Therefore, the unknown parameters can be derived from those obtained in experiments by building numerical climate models of general or global atmospheric circulation (GCMs). The majority of the well known models are based on numerical solution of the 3D equations of geophysical fluid dynamics (GFD).

One of the first attempts to numerically describe the atmosphere of Mars was made by Leovy and Mintz (1969) [2], who successfully adapted the GCM developed at the University of California (Los Angeles) to the Martian conditions. Since then, Martian GCMs proliferated. To date, there are several models of sufficient complexity, which were developed in the United States, France, Britain, Japan, Canada, and Germany. They are used for investigation of a wide range of processes and phenomena in the Martian atmosphere and for interpretation of observational data. The availability of plentiful measurements of water vapor stimulated attempts to simulate the water cycle with the Martian GCMs.

Water in its different phases is a very important element of the current Martian climate, being a sensitive marker of meteorology in the atmosphere. It affects the Martian climate mostly through radiative effects of water ice clouds and scavenging dust from the atmosphere. Water was first detected in the Martian atmosphere more than a half century ago [3]. The next generation of studies broadly utilized data from orbiting and landing spacecraft, e.g., from Mars Atmospheric Water Detector (MAWD) onboard the Viking Orbiter [4]. To date, the main sources of information about the water distribution in the Martian atmosphere are the Thermal Emission Spectrometer (TES) onboard Mars Global Surveyor (MGS) [5; 6], the Mars Climate Sounder (MCS) and the Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) onboard Mars Reconnaissance Orbiter (MRO) [7], the LIDAR instrument onboard the Phoenix Lander [8] and the Planetary Fourier Spectrometer (PFS), the Visible and Infrared Mineralogical Mapping Spectrometer (OMEGA), the Spectroscopy for Investigation of Characteristics of the Atmosphere of Mars (SPICAM) instruments onboard Mars Express [9—15] and the Atmospheric Chemistry Suite (ACS) and Nadir and Occultation for Mars Discovery (NOMAD) instruments onboard ExoMars Trace Gas Orbiter (TGO) [16].

The history of the water cycle modeling starts from the work of Davies (1981) [17] who has developed a model to test the hypothesis that the observed seasonal and latitudinal distribution of water on Mars is controlled by sublimation and condensation of surface ice deposits in the polar regions, and by the meridional transport of water vapor. Then, James (1990) [18] used a 1D model to show the role of water ice clouds in the water migration from north to south. The first comprehensive microphysical model of clouds was developed by Michelangeli et al. (1993) [19] following the earlier attempts undertaken after measurements of water vapor vertical profiles [20]. Colaprete et al. (1999) [21] used microphysical models and Haberle et al. (1999) [22] employed a Martian general circulation model (MGCM) to reproduce observations provided by Mars Pathfinder. Richardson and Wilson (2002) [23] and Richardson et al. (2002) [24] used the Geophysical Fluid Dynamics Laboratory (GFDL) MGCM to simulate the annual water cycle on Mars and compared it with the Viking MAWD data. Although the simulated climate was overly wet, these studies revealed the key mechanisms of the water transport. A more sophisticated model, which included

transport, phase transitions and microphysical processes, has been developed by Montmessin et al. (2004) [25]. Later a microphysical model for Mars dust and ice clouds has been applied in combination with a model of the planetary boundary layer (PBL) for interpretation of measurements by the LIDAR instrument on the Phoenix Mars lander [26]. Observations of temperature inversions in the atmosphere of Mars [27] have motivated modelers to include effects of radiatively active water ice clouds (RAC) in MGCMs [28—32]. These studies have demonstrated that accounting for RAC helped to reduce global temperature biases between simulations and observations at northern spring and summer [33]. More MGCMs that include water cycle have been developed to date: DRAMATIC (Dynamics, RAdiation, MAterial Transport and their mutual InteraCtions) MGCM [34], NASA Ames GCM [35], GEM-Mars (The Global Environmental Multiscale model for Mars) GCM [36], the Laboratoire de Meteorologie Dynamique (LMD) MGCM [25; 37] and the Oxford University MGCM [38]. The cloud scheme described by Montmessin et al. (2004) [25] was implemented at least in the latter two models, while the Oxford MGCM also used data assimilation scheme to nudge the simulated temperature to available observations.

In order to successfully reproduce water cloud formations in the atmosphere of Mars, microphysical models require a correct prediction of the size distribution of aerosol particles, which serve as cloud condensation nuclei (CCN). Several observations have provided the evidence that this distribution is bimodal [39—41]. The distribution is called bimodal if its density function has two peaks, or modes. Montmessin et al. (2002) [42] implemented such distribution into their one-dimensional model, prescribing two peaks with constant effective radii and variance for fine and large modes with a fixed ratio between them. They indicated that this assumption improved the simulations. For instance, it resulted in decrease of the effective radii of ice particles condensing on the CCN. In the second chapter of this study, we focus on the effects of the bimodal dust distribution on the global hydrological cycle.

As it was stated, water is a minor component of the Martian atmosphere, which is largely confined within a few lower scale heights. Nevertheless, it is also the main source of hydrogen in the upper atmosphere [43—45]. Escape of hydrogen atoms into space near the exobase varies by an order of magnitude seasonally,

maximizing around southern summer solstice (solar longitude Ls « 270°), according to MAVEN [46] and HST observations [47] during dust storms [48—51]. Observed water in the lower atmosphere also experiences strong seasonal changes and depends on airborne dust load [7; 14; 15; 32]. This implies a link between water in the troposphere and thermosphere and a corresponding mechanism of transport between the layers.

The Martian middle atmosphere is too cold to sustain water vapor in large amounts, especially around the mesopause, while ice particles are sufficiently heavy and prone to sedimentation. This water behavior is similar to that in the terrestrial middle atmosphere [52]. However, there are multiple observations showing a presence of water vapor in the middle atmosphere at certain locations and times [53; 54]. Heavens et al. (2018) [55] and Fedorova et al. (2018) [54] provided evidence of strong seasonal variations of the globally averaged water abundance and its vertical extension up to 70-80 km at perihelion during the Martian Year 28 (MY28) global dust storm. Hypotheses concerning the mechanism of vertical transport of water include mesoscale deep convection [55], turbulent mixing in the lower atmosphere and/or an unspecified dynamics in the upper atmosphere [56]. General circulation modeling underestimates the hygropause altitude at southern summer solstice to date [32; 57]. The third chapter of this study addresses this gap in knowledge of processes that couple water in the lower and upper atmosphere.

The aims of the present research are to conduct numerical simulations of the Martian hydrological cycle using a state-of-the-art MGCM and investigate 1) the influence of various factors, including the bimodality of dust distribution, on water vapor and ice and 2) the mechanism of water exchange between the lower and upper atmosphere.

To achieve the mentioned goals, it is necessary to solve the following research objectives:

1. Develop a numerical hydrological scheme and implement it in an existing MGCM dynamical core. The comprehensive scheme has to account for advective transport, mixing by diffusion, particle size distribution, sedimentation, spatio-temporal variations of atmospheric dust, water saturation, sublimation, nucleation, ice particle growth and water photodissociation.

2. Simulate the hydrological cycle during several Martian years.

3. Investigate the effects of the bimodal dust size distribution on water cycle.

4. Explain the mechanism of water exchange between the lower and upper atmosphere.

5. Compare the results with existing observational data from orbiters and landers.

The hydrological scheme used in the study is based on the approach from the works of Montmessin et al. (2002, 2004) [25; 42] and Navarro et al. (2014) [37]. It is implemented into the Max Planck Institute (MPI) MGCM (also known as MAOAM - Martian Atmosphere Observation and Modeling). This model with the employed physical parameterizations have been described in detail in the works of Hartogh et al. (2005, 2007) [58; 59] and Medvedev and Hartogh (2007) [60]. The most recent applications of this MGCM along with the current setup are presented in the works of Medvedev et al. (2013, 2015, 2016) [61—63] and Yigit et al. (2015) [64].

Scientific Novelty

There is a number of innovations implemented into the hydrological scheme, which have allowed to obtain absolutely new scientific results.

1. A new accurate bimodal dust parameterization based on the SPICAM observational data has been used. Since, dust plays a key role in the Martian hydrological cycle in the low and middle atmosphere, its precise parameterization is critically important for simulations of water.

2. Simulations with the bimodal dust distribution have been performed with the 3D model for the first time. Previous studies [42] used only one-dimensional models and, thus, could not reproduce the water cycle in detail.

3. The model domain has been extended into the thermosphere up to ^160 km. It is one of the two existing MGCMs covering the atmosphere from the ground to almost the exobase, and the only one that employs accurate parametrization of gravity waves in the middle and upper atmosphere. Coupled with the sophisticated hydrological scheme, the MGCM represents a state-of-the-art extended model.

4. The water photodissociation scheme has been implemented in the model to account for the major mechanism of water supersaturation suppression in the upper atmosphere.

5. Systematic errors of commonly used nucleation and particle growth schemes have been discovered and explored. A way of reducing these errors has been proposed.

To sum up, this is the first modeling study that considers in greatest detail the transport of water from the surface to the thermosphere of Mars and explores its links with the atmospheric dust cycle.

Theoretical and Practical value of the study

The results of hydrological cycle simulations can be used for current and future Mars missions in, at least, three different ways. First, the model produces surface map of ground water ice with the prescribed resolution (5.625° in the current work). It could help in selection of landing sites for landers focusing on ground water ice research. The choice of the landing place under such conditions plays an important role in the success of the missions. Second, the predicted by the model wind, temperature and density can help to optimize the landing operations. Of course, the climate model cannot forecast weather at specific time and point, but it can predict main atmospheric features and their variations. Third, simulated vertical distributions of atmospheric tracers such as water vapor and ice can be used for assisting remote sensing performed from orbiters. Other future applications of the model, like forced climate change, climate evolution, or Martian terraforming, require significant modifications of the scheme, but also could be considered.

Theoretical aspects of the model applications include cross-validations with other GCMs, exploring paleoclimate and evolution, testing climate hypotheses, equations and assumptions used in simulations.

Methodology and research methods

The MPI-MGCM employs a spectral dynamical core to solve the primitive equations of geophysical fluid dynamics on a sphere. The physics and tendencies are calculated on a 3D grid, and then are transformed into spectral coefficients at every time step. In the vertical, the grid is defined in the hybrid ^-coordinate [65] discretized into levels, terrain-following near the surface and pressure based near the top. The horizontal grid is based on the Gauss-Kruger map projection with

32 and 64 bins in latitude and longitude, respectively. This discretization corresponds to a T21 triangular spectral truncation, which is a typical resolution of currently employed MGCMs, with a few exceptions for high-resolution experiments [32; 66; 67]. Finite spatial resolution can be a source of numerically-induced features in simulations, which is discussed in the text.

The spectral dynamical core is not well suited for simulation of the tracer transport. Instead, the advection scheme based on a semi-Lagrangian explicit monotonous second-order hybrid scheme and the time splitting method in three spatial directions [68] are adopted. 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 [69]. In addition to advection, transport includes diffusion and mixing associated with subgrid-scale processes. The importance of vertical eddy mixing for modeling the water cycle was emphasized by Richardson and Wilson (2002) [23]. In our simulations, the Crank-Nicolson implicit method with the Richardson number-based diffusion coefficients is used [70] to solve the vertical diffusion equation.

The results of simulations have been validated with observational data obtained from TES, SPICAM, CRISM, MCS and other instruments.

Statements to be defended:

1. A new microphysical scheme for water cycle on Mars implemented in a 3D general circulation model.

2. Accounting for bi-modality of aerosol particle size distribution improves simulations of water ice characteristics in the model compared to observations.

3. The fine fraction of atmospheric aerosols weakly affects spatial distribution of water vapor in the model.

4. Global circulation modeling reveals the mechanism of water exchange between the lower and upper atmosphere.

5. Atmospheric dust controls the circulation strength and, hence, the amount of high-altitude water.

6. Solar tide modulates the upwelling of water vapor by almost completely shutting it down during certain local times.

Presentation and validation of research results

The reliability of the simulation results is confirmed by comparison with known observational data and the results of other models. The main results of the work were reported at 18 conferences, 9 of which are international, e.g.:

1. International Forum «SpaceKazan-IAPS-2015», Kazan, Russia, 2015;

2. II International Scientific Conference «Science of the Future», Kazan, Russia, 2016;

3. International Scientific Conference «AGU Fall Meeting 2016», San Francisco, United States, 2016;

4. «The Sixth International Workshop on the Mars Atmosphere: Modeling and Observations», Granada, Spain, 2017;

5. International «Les Houches winter school on the planetary atmospheres», Les Houches, France, 2017;

6. International Workshop «6th ACS science working team», Suzdal, Russia, 2018;

7. International Scientific Conference «Asia Oceania Geosciences Society Annual meeting», Hawaii, USA, 2018;

8. The First International Aerospace Symposium «The Silk Road», Moscow, Russia, 2018;

9. International Scientific Conference «AGU Fall Meeting», Washington, USA, 2018.

Publications

The main results of the thesis are presented in 6 publications [69; 71—75], 3 of which are published in refereed journals included in Web of Science and Scopus and recommended by Higher Attestation Commission [69; 71; 72], 3 — in conference proceedings [73—75]. The certificate of state registration of computer program №2019611779 was obtained by the author [76].

Personal Contribution

The program code of the hydrological scheme and aerosol microphysics had been developed and implemented by the author. All numerical experiments had been carried out and processed by him. The author was the first author of all his publications and the correspondence with editorial offices and referees has been

run by him as well. The content of the articles had been written by the author in cooperation with the co-authors.

The amount and structure of the work

The thesis consists of an introduction, four chapters, a summary and conclusions. The full volume of the thesis is 102 pages, including 26 figures and 3 tables. The bibliography contains 135 cites.

This study has been performed at the Laboratory of Applied Infrared Spectroscopy of Moscow Institute of Physics and Technology in cooperation with Max Planck Institute for Solar System Research. The work was partially supported by the Russian Science Foundation Grant 16-12-10559 and German Science Foundation (DFG) Grant HA3261/8-1.

Заключение диссертации по теме «Планетные исследования», Шапошников Дмитрий Сергеевич

Summary and conclusions

Water in its different phases is a very important element of the current Martian climate and a sensitive marker of meteorology in the atmosphere. This work presented a new hydrological scheme implemented in the general circulation model of the Martian atmosphere developed at Moscow Institute of Physics and Technology in cooperation with Max Planck Institute for Solar System Research (Germany). The scheme accounts for advective transport, mixing by diffusion, particle size distribution, sedimentation, spatio-temporal variations of atmospheric dust, water saturation, sublimation, nucleation, ice particle growth and water photodissociation.

The model realistically reproduced the seasonal and spatial distributions of water vapor and ice observed by SPICAM (Mars Express), TES (Mars Global Surveyor), CRISM and MCS (Mars Reconnaissance Orbiter) instruments. Simulated abundances of water vapor, ice and effective radii of ice particles agreed well for individual orbits as well.

Simulations with the extended (up to 160 km) version of the model revealed the water "pump" mechanism of water vapor transport from the Martian lower atmosphere to the thermosphere, and helped to quantify the role of airborne dust and solar tides in it. The results explained recent measurements of hydrogen escape at the exobase obtained from MAVEN and HST. They are also consistent with recent observations from ACS and NOMAD (Trace Gas Orbiter).

The main results of the work are as follows:

1. A new microphysical scheme for water cycle on Mars implemented in a 3D general circulation model.

2. Accounting for bi-modality of aerosol particle size distribution improves simulations of water ice characteristics in the model compared to observations.

3. The fine fraction of atmospheric aerosols weakly affects spatial distribution of water vapor in the model.

4. Global circulation modeling reveals the mechanism of water exchange between the lower and upper atmosphere.

5. Atmospheric dust controls the circulation strength and, hence, the amount of high-altitude water.

6. Solar tide modulates the upwelling of water vapor by almost completely shutting it down during certain local times.

The data supporting the MPI-MGCM simulations can be found at https://mars.mipt.ru, https://zenodo.org/record/1045331 [134], https://zenodo.org/record/1553514 [135] or obtained from the author ([e-mail]).

Acknowledgements

First of all, the author wants to thank his supervisor, Alexander Rodin, for his unprecedented assistance in preparing this thesis, for his leadership in research, for his advice on the preparation of articles and control over the content.

The author also expresses deep gratitude to his main co-author, Alexander Medvedev, for his invaluable assistance in preparing articles, for his advice and improvement of the text, for his suggestions on the development of this study.

Also, the author would like to thank Alexander Trokhimovskiy, Anna Fedorova and Daria Betsis for providing access to SPICAM data, as well as for assistance in interpreting the results.

The author expresses gratitude to Chris Mockel, Takeshi Kuroda, Nicholas Heavens and Scott Guzewich for assistance with other observational data and helpful discussions.

And last but not least, the author would like to thank his family for the support during this study. I love you, thank you!

Список литературы диссертационного исследования кандидат наук Шапошников Дмитрий Сергеевич, 2019 год

Bibliography

1. Sheehan, W. The planet Mars: A history of observation & discovery / W. Shee-han. — University of Arizona Press, 1996.

2. Leovy, C. Numerical simulation of the atmospheric circulation and climate of Mars / C. Leovy, Y. Mintz // Journal of the Atmospheric Sciences. — 1969. - Vol. 26, no. 6. - P. 1167-1190.

3. Spinrad, H. The detection of water vapor on Mars / H. Spinrad, G. Münch, L. Kaplan // The Astrophysical Journal. — 1963. — Vol. 137, no. 4. — P. 1319-1321.

4. Jakosky, B. M. The seasonal and global behavior of water vapor in the Mars atmosphere: Complete global results of the Viking atmospheric water detector experiment / B. M. Jakosky, C. B. Farmer // Journal of Geophysical Research. - 1982. - Vol. 87, B4. - P. 2999-3019.

5. Thermal Emission Spectrometer results' Mars atmospheric thermal structure and aerosol distribution / M. D. Smith [et al.] // Journal of Geophysical Research. - 2001. - Vol. 106945, no. 25. - P. 929-23.

6. Smith, M. D. Interannual variability in TES atmospheric observations of Mars during 1999-2003 / M. D. Smith // Icarus. - 2004. - Vol. 167, no. 1. -P. 148-165.

7. Compact Reconnaissance Imaging Spectrometer observations of water vapor and carbon monoxide / M. D. Smith [et al.] // Journal of Geophysical Research. - 2009. - Vol. 114, E2. - E00D03. - URL: http://doi.wiley.com/ 10.1029/2008JE003288.

8. Mars water-ice clouds and precipitation / J. Whiteway [et al.] // science. — 2009. - Vol. 325, no. 5936. - P. 68-70.

9. Mars water vapor abundance from SPICAM IR spectrometer: Seasonal and geographic distributions / A. Fedorova [et al.] // Journal of Geophysical Research E: Planets. - 2006. - Vol. 111, no. 9.

10. Martian water vapor: Mars Express PFS/LW observations / T. Fouchet [et al.] // Icarus. - 2007. - Vol. 190, no. 1. - P. 32-49.

11. Water vapor mapping on Mars using OMEGA/Mars Express / R. Melchiorri [et al.] // Planetary and Space Science. — 2007. — Vol. 55, no. 3. — P. 333-342.

12. Investigation of water vapor on Mars with PFS/SW of Mars Express / M. Tschimmel [et al.] // Icarus. - 2008. - Vol. 195, no. 2. - P. 557-575.

13. Sindoni, G. Observations of water vapour and carbon monoxide in the Martian atmosphere with the SWC of PFS/MEX / G. Sindoni, V. Formisano, A. Geminale // Planetary and Space Science. — 2011. — Vol. 59, no. 2/3. — P. 149-162.

14. Annual survey of water vapor behavior from the OMEGA mapping spectrometer onboard Mars Express / L. Maltagliati [et al.] // Icarus. — 2011. — Vol. 213, no. 2. - P. 480-495.

15. Mars' water vapor mapping by the SPICAM IR spectrometer: Five martian years of observations / A. Trokhimovskiy [et al.] // Icarus. — 2015. — Vol. 251. - P. 50-64.

16. Martian dust storm impact on atmospheric H 2 O and D/H observed by ExoMars Trace Gas Orbiter / A. C. Vandaele [et al.] // Nature. — 2019. — Vol. 568, no. 7753. - P. 521.

17. Davies, D. W. The Mars water cycle / D. W. Davies // Icarus. — 1981. — Vol. 45, no. 2. - P. 398-414.

18. James, P. B. The role of water ice clouds in the Martian hydrologic cycle / P. B. James // Journal of Geophysical Research: Solid Earth. — 1990. — Vol. 95, B2. - P. 1439-1445.

19. Numerical simulations of the formation and evolution of water ice clouds in the Martian atmosphere / D. V. Michelangeli [et al.] // Icarus. — 1993. — Vol. 102, no. 2. - P. 261-285. - URL: http://adsabs.harvard.edu/cgi-bin/nph-bib%7B%5C_%7Dquery?bibcode=1993Icar..102..261M%7B%5C& %7Ddb%7B%5C_%7Dkey=AST.

20. Kulikov, I. N. Modeling of the vertical distribution of water in the atmosphere of Mars / I. N. Kulikov, M. V. Rykhletskii // Astronomicheskii Vestnik. — 1984. - Vol. 17. - P. 112-118.

21. Colaprete, A. Cloud formation under Mars Pathfinder conditions / A. Co-laprete, O. B. Toon, J. A. Magalhaes // Journal of Geophysical Research. — 1999. - Vol. 104, E4. - P. 9043. - URL: http://doi.wiley.com/10.1029/ 1998JE900018.

22. General circulation model simulations of the Mars Pathfinder atmospheric structure investigation/meteorology data / R. M. Haberle [et al.] // Journal of Geophysical Research. - 1999. - Vol. 104, E4. - P. 8957.

23. Richardson, M. I. Investigation of the nature and stability of the Martian seasonal water cycle with a general circulation model / M. I. Richardson, R. J. Wilson // Journal of Geophysical Research. — 2002. — Vol. 107, E5. — P. 5031. - URL: http://adsabs.harvard.edu/abs/2002JGRE..107.5031R.

24. Richardson, M. I. Water ice clouds in the Martian atmosphere: General circulation model experiments with a simple cloud scheme / M. I. Richardson, R. J. Wilson, A. V. Rodin // Journal of Geophysical Research. — 2002. — Vol. 107, E9. - P. 5064. - URL: http://doi.wiley.com/ 10.1029/ 2001JE001804.

25. Origin and role of water ice clouds in the Martian water cycle as inferred from a general circulation model / F. Montmessin [et al.] //J. Geophys. Res. — 2004. - Vol. 109, E10004. - P. 1-26.

26. Simulating observed boundary layer clouds on Mars / F. Daerden [et al.] // Geophysical Research Letters. — 2010. — Vol. 37, no. 4.

27. Hinson, D. P. Temperature inversions, thermal tides, and water ice clouds in the Martian tropics / D. P. Hinson, R. J. Wilson // Journal of Geophysical Research. - 2004. - Vol. 109, E1. - E01002. - URL: http://doi.wiley. com/10.1029/2003JE002129.

28. Wilson, R. J. Diurnal variation and radiative influence of Martian water ice clouds / R. J. Wilson, G. A. Neumann, M. D. Smith // Geophysical Research Letters. - 2007. - Vol. 34, no. 2.

29. Influence of water ice clouds on Martian tropical atmospheric temperatures: MARTIAN WATER ICE CLOUDS / R. J. Wilson [et al.] // Geophysical Research Letters. — 2008. — Vol. 35, no. 7. — n/a—n/a. — URL: http : / / doi . wiley. com / 10 . 1029 / 2007GL032405 % 7B % 5C % %7D5Cnhttp : / / onlinelibrary. wiley. com / store / 10 . 1029 / 2007GL032405 / asset / grl24098. pdf ? v = 1 % 7B % 5C & %7Dt = i1dc94tt % 7B % 5C & %7Ds = 49c440b27fd227263e14d5f18d4c5bd8e4fa70d6.

30. Radiative Effects of Water Ice Clouds on the Martian Seasonal Water Cycle . / R. M. Haberle [et al.] // Forth International Workshop on the Mars Atmosphere: Modelling and observations. — Laboratoire de Météorologie Dynamique. Paris, France, 2011. — P. 223—226.

31. The influence of radiatively active water ice clouds on the Martian climate / J. B. Madeleine [et al.] // Geophysical Research Letters. — 2012. — Vol. 39, no. 23.

32. Unraveling the Martian water cycle with high-resolution global climate simulations / A. Pottier [et al.] // Icarus. - 2017. - Vol. 291. - P. 82-106.

33. Urata, R. A. Simulations of the martian hydrologic cycle with a general circulation model: Implications for the ancient martian climate / R. A. Urata, O. B. Toon // Icarus. - 2013. - Vol. 226, no. 1. - P. 229-250.

34. Kuroda, T. Simulation of the Water Cycle Including HDO/H2O Isotopic Fractionation on the Present Mars Using Dramatic MGCM / T. Kuroda // Sixth International Workshop on the Mars Atmosphere: Modelling and Observations. — Instituto de Astrofísica de Andalucía. Granada, Spain, 2017.

35. Updates on Modeling the Water Cycle with the NASA Ames Mars Global Climate Model / M. A. Kahre [et al.] // Sixth International Workshop on the Mars Atmosphere: Modelling and Observations. — Instituto de Astrofísica de Andalucía. Granada, Spain, 2017.

36. Neary, L. The GEM-Mars general circulation model for Mars: Description and evaluation / L. Neary, F. Daerden // Icarus. — 2018. — Vol. 300. — P. 458-476.

37. Global climate modeling of the Martian water cycle with improved micro-physics and radiatively active water ice clouds / T. Navarro [et al.] // Journal of Geophysical Research: Planets. — 2014. — Vol. 119, no. 7. — P. 1479-1495.

38. The seasonal cycle of water vapour on Mars from assimilation of thermal emission spectrometer data / L. Steele [et al.] // Icarus. — 2014. — Vol. 237. — P. 97-115.

39. Stellar occultations at UV wavelengths by the SPICAM instrument: Retrieval and analysis of Martian haze profiles / F. Montmessin [et al.] // Journal of Geophysical Research E: Planets. — 2006. — Vol. 111, no. 9.

40. A complete climatology of the aerosol vertical distribution on Mars from MEx/SPICAM UV solar occultations / A. Määttänen [et al.] // Icarus. — 2013. - Vol. 223, no. 2. - P. 892-941.

41. Evidence for a bimodal size distribution for the suspended aerosol particles on mars / A. A. Fedorova [et al.] // Icarus. - 2014. - Vol. 231. - P. 239-260.

42. Montmessin, F. New insights into Martian dust distribution and water-ice cloud microphysics / F. Montmessin, P. Rannou, M. Cabine // Journal of Geophysical Research. - 2002. - Vol. 107, E6. - P. 5037. - URL: http: //doi.wiley.com/10.1029/2001JE001520.

43. Hunten, D. Production and escape of hydrogen on Mars / D. Hunten, M. McElroy // Journal of Geophysical Research. — 1970. — Vol. 75, no. 31. — P. 5989-6001.

44. Parkinson, T. Spectroscopy and acronomy of O2 on Mars / T. Parkinson, D. Hunten // Journal of the Atmospheric Sciences. — 1972. — Vol. 29, no. 7. - P. 1380-1390.

45. Krasnopolsky, V. A. Mars' upper atmosphere and ionosphere at low, medium, and high solar activities: Implications for evolution of water / V. A. Krasnopolsky // Journal of Geophysical Research: Planets. — 2002. — Vol. 107, E12. - P. 11-1.

46. Halekas, J. Seasonal variability of the hydrogen exosphere of Mars / J. Halekas // Journal of Geophysical Research: Planets. — 2017. — Vol. 122, no. 5. - P. 901-911.

47. Seasonal changes in hydrogen escape from mars through analysis of HST observations of the Martian exosphere near perihelion / D. Bhattacharyya [et al.] // Journal of Geophysical Research: Space Physics. — 2017. — Vol. 122, no. 11.

48. A strong seasonal dependence in the Martian hydrogen exosphere / D. Bhattacharyya [et al.] // Geophysical Research Letters. — 2015. — Vol. 42, no. 20. - P. 8678-8685.

49. Unexpected variability of Martian hydrogen escape / M. S. Chaffin [et al.] // Geophysical Research Letters. - 2014. - Vol. 41, no. 2. - P. 314-320.

50. A rapid decrease of the hydrogen corona of Mars / J. T. Clarke [et al.] // Geophysical Research Letters. - 2014. - Vol. 41, no. 22. - P. 8013-8020.

51. Variability of D and H in the Martian upper atmosphere observed with the MAVEN IUVS echelle channel / J. T. Clarke [et al.] // Journal of Geophysical Research: Space Physics. - 2017. - Vol. 122, no. 2. - P. 2336-2344. -URL: https : / / agupubs . onlinelibrary. wiley. com / doi / abs / 10 . 1002 / 2016JA023479.

52. Seele, C. Water vapor of the polar middle atmosphere: Annual variation and summer mesosphere Conditions as observed by ground-based microwave spectroscopy / C. Seele, P. Hartogh // Geophysical Research Letters. — 1999. - Vol. 26, no. 11. - P. 1517-1520. - eprint: https://agupubs. onlinelibrary.wiley.com/doi/pdf/10.1029/1999GL900315. - URL: https: //agupubs.onlinelibrary.wiley.com/doi/abs/10.1029/1999GL900315.

53. Annual survey of water vapor vertical distribution and water-aerosol coupling in the martian atmosphere observed by SPICAM/MEx solar occultations / L. Maltagliati [et al.] // Icarus. - 2013. - Vol. 223, no. 2. - P. 942-962.

54. Water vapor in the middle atmosphere of Mars during the 2007 global dust storm / A. Fedorova [et al.] // Icarus. - 2018. - Vol. 300. - P. 440-457.

55. Hydrogen escape from Mars enhanced by deep convection in dust storms / N. G. Heavens [et al.] // Nature Astronomy. — 2018. - Vol. 2, no. 2. -P. 126.

56. Clarke, J. T. Dust-enhanced water escape / J. T. Clarke // Nature Astronomy. - 2018. - Vol. 2, no. 2. - P. 114.

57. Variability of the hydrogen in the martian upper atmosphere as simulated by a 3D atmosphere-exosphere coupling / J.-Y. Chaufray [h gp.] // Icarus. — 2015. — T. 245. — C. 282—294. — URL: http://www.sciencedirect.com/ science/article/pii/S0019103514004540.

58. Description and climatology of a new general circulation model of the Martian atmosphere / P. Hartogh [et al.] // Journal of Geophysical Research. — 2005. - Vol. 110, E11. -E11008. - URL: http://doi.wiley.com/10.1029/ 2005JE002498.

59. Hartogh, P. Middle atmosphere polar warmings on Mars: Simulations and study on the validation with sub-millimeter observations / P. Hartogh, A. S. Medvedev, C. Jarchow // Planetary and Space Science. — 2007. — Vol. 55, no. 9. - P. 1103-1112.

60. Medvedev, A. S. Winter polar warmings and the meridional transport on Mars simulated with a general circulation model / A. S. Medvedev, P. Hartogh // Icarus. - 2007. - Vol. 186, no. 1. - P. 97-110.

61. General circulation modeling of the Martian upper atmosphere during global dust storms / A. S. Medvedev [et al.] // Journal of Geophysical Research: Planets. - 2013. - Vol. 118, no. 10. - P. 2234-2246.

62. Cooling of the Martian thermosphere by CO2 radiation and gravity waves: An intercomparison study with two general circulation models / A. S. Medvedev [et al.] // Journal of Geophysical Research E: Planets. — 2015. — Vol. 120, no. 5. - P. 913-927. — arXiv: arXiv: 1504.05550v1. - URL: http://doi. wiley.com/10.1002/2015JE004802.

63. Comparison of the Martian thermospheric density and temperature from IUVS/MAVEN data and general circulation modeling / A. S. Medvedev [et al.] // Geophysical Research Letters. — 2016. — Vol. 43, no. 7. — P. 3095-3104.

64. Yigit, E. Gravity waves and high-altitude CO2 ice cloud formation in the Martian atmosphere / E. Yigit, A. S. Medvedev, P. Hartogh // Geophysical Research Letters. - 2015. - Vol. 42, no. 11. - P. 4294-4300. - URL: http://doi.wiley.com/10.1002/2015GL064275.

65. Simmons, A. J. An Energy and Angular-Momentum Conserving Vertical Finite-Difference Scheme and Hybrid Vertical Coordinates / A. J. Simmons, D. M. Burridge // Monthly Weather Review. — 1981. — Vol. 109, no. 4. — P. 758—766. — URL: http://journals.ametsoc.org/doi/abs/10.1175/1520-0493%7B%5C%%7D281981%7B%5C%%7D29109%7B%5C%%7D3C0758% 7B%5C%%7D3AAEAAMC%7B%5C%%7D3E2.0.CO%7B%5C%%7D3B2.

66. A global view of gravity waves in the Martian atmosphere inferred from a high-resolution general circulation model / T. Kuroda [et al.] // Geophysical Research Letters. - 2015. - Vol. 42, no. 21. - P. 9213-9222.

67. Global distribution of gravity wave sources and fields in the Martian atmosphere during equinox and solstice inferred from a high-resolution general circulation model / T. Kuroda [et al.] // Journal of the Atmospheric Sciences. - 2016. - Vol. 73, no. 12. - P. 4895-4909.

68. Generalization of the hybrid monotone second-order finite difference scheme for gas dynamics equations to the case of unstructured 3D grid / V. S. Min-galev [et al.] // Computational Mathematics and Mathematical Physics. — 2010. - Vol. 50, no. 5. - P. 877-889. - URL: http://link.springer.com/10. 1134/S0965542510050118.

69. Shaposhnikov, D. S. The water cycle in the general circulation model of the martian atmosphere / D. S. Shaposhnikov, A. V. Rodin, A. S. Medvedev // Solar System Research. - 2016. - Vol. 50, no. 2. - P. 90-101.

70. Becker, E. Nonlinear Horizontal Diffusion for GCMs / E. Becker, U. Burkhardt // Monthly Weather Review. — 2007. — Vol. 135, no. 4. — P. 1439—1454. — URL: http://journals.ametsoc.org/doi/abs/10.1175/ MWR3348.1.

71. Modeling the hydrological cycle in the atmosphere of Mars: Influence of a bimodal size distribution of aerosol nucleation particles / D. S. Shaposhnikov [et al.] // Journal of Geophysical Research: Planets. — 2018. — Vol. 123, no. 2. - P. 508-526.

72. Seasonal Water "Pump" in the Atmosphere of Mars: Vertical Transport to the Thermosphere / D. S. Shaposhnikov [et al.] // Geophysical Research Letters. - 2019. - Vol. 46. - P. 4161-4169.

73. Shaposhnikov, D. S. Fazovye prevrashhenija i obmen vody mezhdu atmosferoj i poverhnost'ju v chislennoj modeli obshhej cirkuljacii atmosfery Marsa [Phase transformations and water exchange between the atmosphere and the surface in the general circulation numerical model of the Martian atmosphere] / D. S. Shaposhnikov, A. V. Rodin // Problemy sovremennoj fiziki. Trudy 57-j nauchnoj konferencii MFTI [Problems of modern physics. Proceedings of the 57th Scientific Conference of MIPT]. - 2014. - P. 197-198.

74. Shaposhnikov, D. S. Diffuzija passivnoj primesi v gidrologicheskom cikle modeli obshhej cirkuljacii atmosfery Marsa MAOAM [Diffusion of a passive tracer in the hydrological cycle of the Martian general atmosphere circulation model MAOAM] / D. S. Shaposhnikov, A. V. Rodin, A. S. Medvedev // Sovre-mennye problemy distancionnogo zondirovanija Zemli iz kosmosa [Modern problems of remote sensing of the Earth from space]. — 2016. — P. 223—223.

75. Shaposhnikov, D. S. Gidrologicheskij cikl v chislennoj modeli obshhej cirkuljacii atmosfery Marsa [Hydrological cycle in the general circulation numerical model of the Marian atmosphere] / D. S. Shaposhnikov, A. V. Rodin, A. S. Medvedev // Problemy sovremennoj fiziki. Trudy 59-j nauchnoj konfer-encii MFTI [Problems of modern physics. Proceedings of the 59th Scientific Conference of MIPT]. - 2016. - P. 37-38.

76. Shaposhnikov, D. S. Blok gidrologicheskogo cikla v chislennoy modeli global'noy cirkuljacii atmosfery Marsa [The hydrological cycle block in the numerical model of the global circulation of the atmosphere of Mars] // Certificate of state registration of computer programs № 2019611779 (date of registration 04.02.2019) / D. S. Shaposhnikov. — 2019.

77. Williams, D. R. Mars fact sheet / D. R. Williams // https://nssdc.gsfc.nasa.gov/pli 2004.

78. Moroz, V. I. Novyye issledovaniya Marsa i sravnitelnaya planetologiya [New Mars Research and Comparative Planetology] / V. I. Moroz, O. I. Korablev,

A. V. Rodin // Priroda [Nature]. - 2005. - No. 9. - P. 25-33.

79. Laskar, J. Orbital forcing of the Martian polar layered deposits / J. Laskar,

B. Levrard, J. F. Mustard // Nature. - 2002. - Vol. 419, no. 6905. - P. 375.

80. Mars: a small terrestrial planet / N. Mangold [et al.] // The Astronomy and Astrophysics Review. — 2016. — Vol. 24, no. 1. — P. 15.

81. Moroz, V. The atmosphere of Mars / V. Moroz // Space Science Reviews. — 1976. - Vol. 19, no. 6. - P. 763-843.

82. On the possibility of liquid water on present-day Mars / R. M. Haberle [et al.] // Journal of Geophysical Research: Planets. — 2001. — Vol. 106, E10. - P. 23317-23326.

83. Hoffman, N. White Mars: A new model for Mars' surface and atmosphere based on CO2 / N. Hoffman // Icarus. - 2000. - Vol. 146, no. 2. -P. 326-342.

84. Water vapor saturation at low altitudes around Mars aphelion: A key to Mars climate? / R. Clancy [et al.] // Icarus. - 1996. - Vol. 122, no. 1. -P. 36-62.

85. Jakosky, B. M. The seasonal behavior of water on Mars / B. M. Jakosky, R. M. Haberle // Mars. - 1992. - P. 969-1016.

86. Present-day Mars' water cycle: new views and blind perspectives / F. Montmessin [h gp.] // European Planetary Science Congress 2012. — 2012.

87. Kutepov, A. Solution of the non-LTE problem for molecular gas in planetary atmospheres: superiority of accelerated lambda iteration / A. Kutepov, O. Gusev, V. Ogibalov // Journal of Quantitative Spectroscopy and Radiative Transfer. - 1998. - Vol. 60, no. 2. - P. 199-220. - URL: http: //linkinghub.elsevier.com/retrieve/pii/S0022407397001672.

88. Hoskins, B. A multi-layer spectral model and the semi-implicit method / B. Hoskins, A. Simmons // Quarterly Journal of the Royal Meteorological Society. - 1975. - Vol. 101, no. 429. - P. 637-655.

89. Asselin, R. Frequency filter for time integrations / R. Asselin // Mon. Wea. Rev. - 1972. - Vol. 100, no. 6. - P. 487-490.

90. Report of the Kuhlungsborn Mechanistic Circulation Model : tech. rep. / E. Becker [et al.] ; Leibniz Institute of Atmospheric Physics, Kuhlungsborn, Germany. - 2010. - P. 97.

91. Influence of gravity waves on the Martian atmosphere: General circulation modeling / A. S. Medvedev [et al.] // Journal of Geophysical Research: Planets. -2011. - Vol. 116, E10.

92. Conrath, B. J. Thermal structure of the Martian atmosphere during the dissipation of the dust storm of 1971 / B. J. Conrath // Icarus. — 1975. — Vol. 24, no. 1. - P. 36-46.

93. Rodin, A. V. On the moment method for the modeling of cloud microphysics in rarefied turbulent atmospheres: I. Condensation and mixing / A. V. Rodin // Solar System Research. - 2002. - Vol. 36, no. 2. - P. 97-106.

94. Vertical structure of Martian dust measured by solar infrared occultations from the Phobos spacecraft / O. Korablev [et al.] // Icarus. — 1993. — Vol. 102, no. 1. — P. 76—87. — URL: http://linkinghub.elsevier.com/ retrieve/doi/10.1006/icar.1993.1033.

95. Burlakov, a. V. A one-dimensional numerical model of H2O cloud formation in the Martian atmosphere / a. V. Burlakov, a. V. Rodin // Solar System Research. - 2012. - Vol. 46, no. 1. - P. 18-30. - URL: http://link. springer.com/10.1134/S0038094611060037.

96. Numerical simulations of the three-dimensional distribution of meteoric dust in the mesosphere and upper stratosphere / C. G. Bardeen [et al.] // Journal of Geophysical Research Atmospheres. — 2008. — Vol. 113, no. 17.

97. Kok, J. F. Enhancement of the emission of mineral dust aerosols by electric forces / J. F. Kok, N. O. Renno // Geophysical Research Letters. — 2006. — Vol. 33, no. 19. - L19S10. - URL: http://doi.wiley.com/ 10.1029/ 2006GL026284.

98. Curry, J. A. Thermodynamics of atmospheres and oceans. Vol. 65 / J. A. Curry, P. J. Webster. — London, UK : Academic Press, 1998.

99. Jacobson, M. Z. Fundamentals of Atmospheric Modeling / M. Z. Jacobson. — Cambridge, UK : Cambridge University Press, 2005.

100. Trainer, M. G. Measurements of depositional ice nucleation on insoluble substrates at low temperatures: Implications for earth and mars / M. G. Trainer, O. B. Toon, M. A. Tolbert // Journal of Physical Chemistry C. - 2009. -Vol. 113, no. 6. - P. 2036-2040.

101. Water ice cloud formation on Mars is more difficult than presumed: Laboratory studies of ice nucleation on surrogate materials / L. T. Iraci [et al.] // Icarus. - 2010. - Vol. 210, no. 1. - P. 985-991. - URL: https://doi.org/ 10.1016/j.icarus.2010.07.020.

102. Maattanen, A. Estimating the variability of contact parameter temperature dependence with the Monte Carlo Markov Chain method / A. Maattanen, M. Douspis // GeoResJ. - 2014. - Vol. 3/4, no. 1. - P. 46-55.

103. Murphy, D. M. Review of the vapour pressures of ice and supercooled water for atmospheric applications / D. M. Murphy, T. Koop // Quarterly Journal of the Royal Meteorological Society. — 2005. — Vol. 131, no. 608. — P. 1539-1565. - URL: http://doi.wiley.com/10.1256/qj.04.94.

104. Gori, F. Theoretical prediction of the thermal conductivity and temperature variation inside mars soil analogues / F. Gori, S. Corasaniti // Planetary and Space Science. - 2004. - Vol. 52, no. 1-3. - P. 91-99.

105. Water accomodation and desorption kinetics on ice / X. R. Kong [et al.] // J. Phys. Chem. A. - 2014. - Vol. 118, no. 22. - P. 3973-3979.

106. Water vapor measurements at ALOMAR over a solar cycle compared with model calculations by LIMA / P. Hartogh [et al.] // Journal of Geophysical Research: Atmospheres. — 2010. — Vol. 115, no. D1. — eprint: https: //agupubs.onlinelibrary.wiley.com/doi/pdf/10.1029/2009JD012364. - URL: https://agupubs.onlinelibrary.wiley.com/doi/abs/10.1029/2009JD012364.

107. Nicolet, M. Aeronomical aspects of mesospheric photodissociation: Processes resulting from the solar H Lyman-alpha line / M. Nicolet // Planetary and space science. — 1985. — Vol. 33, no. 1. — P. 69—80.

108. Anbar, A. Photodissociation in the atmosphere of Mars: Impact of high resolution, temperature-dependent CO2 cross-section measurements / A. Anbar, M. Allen, H. Nair // Journal of Geophysical Research: Planets. — 1993. — Vol. 98, E6. - P. 10925-10931.

109. Kley, D. Ly(a) absorption cross-section of H2O and O2 / D. Kley // Journal of Atmospheric Chemistry. - 1984. - Vol. 2, no. 2. - P. 203-210.

110. Lean, J. Variability of the Lyman alpha flux with solar activity / J. Lean, A. Skumanich // Journal of Geophysical Research: Space Physics. — 1983. — Vol. 88, A7. - P. 5751-5759.

111. Watanabe, K. Absorption coefficients of gases in the vacuum ultraviolet / K. Watanabe, E. C. Inn, M. Zelikoff // The Journal of Chemical Physics. — 1952. - Vol. 20, no. 12. - P. 1969-1970.

112. Mars Atmospheric Dynamics as Simulated by the NASA Ames General Circulation Model 2. Transient Baroclinic Eddies / J. R. Barnes [et al.] // JOURNAL OF GEOPHYSICAL RESEARCH. - 1993. - Vol. 98, E2. -P. 3125-3148.

113. Seasonal changes of the baroclinic wave activity in the northern hemisphere of Mars simulated with a GCM / T. Kuroda [et al.] // Geophysical research letters. - 2007. - Vol. 34, no. 9.

114. Heterogeneous chemistry in the atmosphere of Mars / F. Lefevre [et al.] // Nature. - 2008. - Vol. 454, no. 7207. - P. 971-975. - URL: http: //www.nature.com/doifinder/10.1038/nature07116.

115. Water in Mars atmosphere: comparison of recent data sets / O. Korablev [et al.] // Mars Atmosphere Modelling and Observations. — 2006. — P. 244. — URL: http://adsabs.harvard.edu/abs/2006mamo.conf..244K.

116. Warren, S. G. Visible and near-ultraviolet absorption spectrum of ice from transmission of solar radiation into snow / S. G. Warren, R. E. Brandt, T. C. Grenfell // Applied Optics. - 2006. - Vol. 45, no. 21. - P. 5320. -URL: http : / / www . ncbi. nlm . nih . gov / pubmed / 16826269 % 7B % 5C % %7D5Cnhttps://www.osapublishing.org/abstract.cfm?URI=ao-45-21-5320.

117. Smith, M. D. The annual cycle of water vapor on Mars as observed by the Thermal Emission Spectrometer / M. D. Smith // Journal of Geophysical Research: Planets. - 2002. - Vol. 107, E11. - P. 25-1-25-19. - URL: http://doi.wiley.com/10.1029/2001JE001522.

118. Richardson, M. I. A general circulation model study of the Mars water cycle : PhD thesis / Richardson Mark Ian. — 1999.

119. Traveling waves in the martian atmosphere from MGS TES Nadir data / D. Banfield [et al.] // Icarus. - 2004. - Vol. 170, no. 2. - P. 365-403. -URL: http://apps.isiknowledge.com/full%7B%5C_%7Drecord.do?product= UA % 7B % 5C & %7Dsearch % 7B % 5C _ %7Dmode = GeneralSearch % 7B % 5C & %7Dqid = 1 % 7B % 5C & %7DSID = S2Dc15im1LK9nOJcIfb % 7B % 5C & %7Dpage=1%7B%5C&%7Ddoc=2%7B%5C&%7Dcolname=WOS.

120. The atmosphere and climate of Mars / R. M. Haberle [et al.]. — Cambridge University Press, 2017.

121. Aerosol properties during the 2007 global dust storm (MY28): Solar infrared occultation observations by SPICAM / D. Betsis [et al.] // 6th IW on the Mars Atmos. — 2017.

122. Guzewich, S. D. The vertical distribution of Martian aerosol particle size / S. D. Guzewich, M. D. Smith, M. J. Wolff // Journal of Geophysical Research: Planets. - 2014. - Vol. 119, no. 12. - P. 2694-2708. - URL: http: //dx.doi.org/10.1002/2014JE004704.

123. Vertical distribution of dust and water ice aerosols from CRISM limb-geometry observations / M. D. Smith [et al.] // Journal of Geophysical Research E: Planets. - 2013. - Vol. 118, no. 2. - P. 321-334.

124. Medvedev, A. S. Influence of dust on the dynamics of the Martian atmosphere above the first scale height / A. S. Medvedev, T. Kuroda, P. Hartogh // Aeolian Research. — 2011. — T. 3, № 2. — C. 145—156. — URL: http://www. sciencedirect.com/science/article/pii/S1875963711000401.

125. On Forcing the Winter Polar Warmings in the Martian Middle Atmosphere during Dust Storms / T. Kuroda [et al.] // Journal of the Meteorological Society of Japan. Ser. II. - 2009. - Vol. 87, no. 5. - P. 913-921.

126. Forbes, J. M. Solar Semidiurnal Tide in the Dusty Atmosphere of Mars / J. M. Forbes, S. Miyahara // Journal of the Atmospheric Sciences. — 2006. — T. 63, №7. — C. 1798—1817. — eprint: https://doi.org/10.1175/JAS3718.!. — URL: https://doi.org/10.1175/JAS3718.1.

127. The semidiurnal tide in the middle atmosphere of Mars / A. Kleinböhl [h gp.] // Geophysical Research Letters. — 2013. — T. 40, № 10. — C. 1952—1959. — eprint: https://agupubs.onlinelibrary.wiley.com/doi/ pdf/10.1002/grl.50497. — URL: https://agupubs.onlinelibrary.wiley.com/ doi/abs/10.1002/grl.50497.

128. Yigit, E. Influence of parameterized small-scale gravity waves on the migrating diurnal tide in Earth's thermosphere / E. Yigit, A. S. Medvedev // Journal of Geophysical Research: Space Physics. — 2017. — T. 122, № 4. — C. 4846—4864. — eprint: https://agupubs.onlinelibrary.wiley.com/doi/ pdf/10. 1002/2017JA024089. — URL: https://agupubs.onlinelibrary.wiley. com/doi/abs/10.1002/2017JA024089.

129. Hallgren, K. First detection of tidal behaviour in polar mesospheric water vapour by ground based microwave spectroscopy / K. Hallgren, P. Hartogh // Atmospheric Chemistry and Physics. — 2012. — Vol. 12, no. 8. — P. 3753-3759. - URL: https://www.atmos-chem-phys.net/12/3753/2012/.

130. Kleinböhl, A. Two-dimensional radiative transfer for the retrieval of limb emission measurements in the Martian atmosphere / A. Kleinböhl, A. J. Friedson, J. T. Schofield // Journal of Quantitative Spectroscopy and Radiative Transfer. - 2017. - Vol. 187. - P. 511-522.

131. Evidence of water vapor in excess of saturation in the atmosphere of Mars / L. Maltagliati [et al.] // Science. - 2011. - Vol. 333, no. 6051. -P. 1868-1871.

132. Elevated atmospheric escape of atomic hydrogen from Mars induced by high-altitude water / M. Chaffin [et al.] // Nature Geoscience. — 2017. — Vol. 10, no. 3. - P. 174.

133. Krasnopolsky, V. A. Photochemistry of water in the martian thermosphere and its effect on hydrogen escape / V. A. Krasnopolsky // Icarus. — 2019. — Т. 321. — С. 62—70. — URL: http://www.sciencedirect.com/science/article/ pii/S0019103518303658.

134. Modeling the hydrological cycle in the atmosphere of Mars: Influence of a bimodal size distribution of aerosol nucleation particles / D. S. Shaposhnikov [et al.]. - 11/2017. - URL: https://doi.org/10.5281/zenodo.1045331.

135. Water "Pump" in the Atmosphere of Mars: Modeling Vertical Transport to the Thermosphere / D. S. Shaposhnikov [et al.]. — 11/2018. — URL: https: //doi.org/10.5281/zenodo.1553514.