scholarly journals Mars: Occurrence of liquid water

1971 ◽  
Vol 40 ◽  
pp. 247-250
Author(s):  
Andrew P. Ingersoll
Keyword(s):  
Liquid Water ◽  
Evaporation Rate ◽  
Heat Sources ◽  
Martian Surface ◽  
Concentrated Solutions ◽  
Water Condensation

In the absence of juvenile liquid water, condensation and subsequent melting of ice are the only means of producing liquid water on the Martian surface. However, the evaporation rate is so high that the available heat sources cannot melt ice on Mars. Melting might occur only in concentrated solutions of strongly deliquescent salts.

scholarly journals Ice on Mars

1974 ◽  
Vol 13 (68) ◽  
pp. 173-185 ◽  
Author(s):  
Robert P. Sharp
Keyword(s):  
Liquid Water ◽  
Polar Regions ◽  
Martian Surface ◽  
Ground Ice ◽  
Water Ice ◽  
Small Areas ◽  
Ice Caps ◽  
The North ◽  
Patterned Structures ◽  
Water Substance

Ice unquestionably exists on Mars. Annual polar-region frost blankets are principally solid CO2, and perennial residual ice caps near each pole are probably water ice, except for a part of the north polar cap which may consist of a 1 km thick mass of solid CO2. Minor amounts of carbon-dioxide clathrate (CO2 · ≈ 6H2O) presumably accompany the solid CO2. The annual frost blankets may have a concentric banding with an outermost very thin layer of water frost, an intermediate narrow zone of clathrate, and a major central core of solid CO2. Layered deposits and underlying homogeneous materials mantle large areas within both polar regions. These blankets are probably composed of dust, volcanic ash, or both, and possibly contain frozen volatiles. They may comprise the largest reservoir of water substance on the Martian surface. Ground ice formed by the freezing of ascending de-gassed water substance may underlie the surface of Mars. Localized collapse of small areas may be due to ground-ice deterioration, and recession of steep slopes may have been caused by ground-ice sapping. If liquid water ever existed in significant quantities on the Martian surface, intense frost shattering, widespread creep, and prolific development of patterned structures should have occurred because the thermal regimen of the surface is highly favorable to the freeze–thaw process. It is ineffective at present owing to the lack of liquid water. No evidence suggests that the residual ice caps have ever acted like terrestrial glaciers in terms of erosion and deposition. Currently, they are too thin, too cold, and presumably frozen to their substrates. Their most important function is to buffer the atmosphere in terms of its H2O and CO2 content, thereby exerting a modifying influence on the surface environment of the entire planet.

scholarly journals Mimicking the Martian Hydrological Cycle: A Set-Up to Introduce Liquid Water in Vacuum

Sensors ◽  
2020 ◽  
Vol 20 (21) ◽  
pp. 6150
Author(s):  
Jesús Manuel Sobrado
Keyword(s):  
Liquid Water ◽  
Vacuum Chamber ◽  
Hydrological Cycle ◽  
Water Cycle ◽  
Technological Development ◽  
Extreme Environment ◽  
Moss Sample ◽  
Water Condensation ◽  
Laboratory Facility ◽  
Set Up

Liquid water is well known as the life ingredient as a solvent. However, so far, it has only been found in liquid state on this planetary surface. The aim of this experiment and technological development was to test if a moss sample is capable of surviving in Martian conditions. We built a system that simulates the environmental conditions of the red planet including its hydrological cycle. This laboratory facility enables us to control the water cycle in its three phases through temperature, relative humidity, hydration, and pressure with a system that injects water droplets into a vacuum chamber. We successfully simulated the daytime and nighttime of Mars by recreating water condensation and created a layer of superficial ice that protects the sample against external radiation and minimizes the loss of humidity due to evaporation to maintain a moss sample in survival conditions in this extreme environment. We performed the simulations with the design and development of different tools that recreate Martian weather in the MARTE simulation chamber.

Combination between Ca, P and Y in the Martian Meteorite NWA 6963 could be used as a strategy to indicate liquid water reservoirs on ancient Mars?

2018 ◽  
Vol 18 (2) ◽  
pp. 151-156 ◽  
Author(s):  
Bruno Leonardo do Nascimento-Dias
Keyword(s):  
Liquid Water ◽  
Hydrothermal Fluids ◽  
Martian Surface ◽  
X Ray ◽  
Geological Characteristics ◽  
The Past ◽  
Northwest Africa ◽  
Aqueous Environments ◽  
Martian Meteorites ◽  
History Of

AbstractAlthough we have learned much about the geological characteristics and history of Mars, the gaps in our knowledge certainly exceed what we understand. Martian meteorites, such as Northwest Africa (NWA) 6963, can be excellent materials for understanding the present and past of Mars, as part of the records of the planet's evolution is preserved in these extraterrestrial rocks. Micro X-ray fluorescence provided data, in which it was possible to verify the presence of Ca, P and Y elements, which are call attention because they were detected superimposed in certain regions. The way these elements were detected indicates the formation of minerals composed by the combination of these elements, such as, for example, Calcite (CaCO3), Apatite [Ca5(PO4)3(OH, F, Cl)], Merrilite [Ca9NaMg (PO4)7] and Xenotime (YPO4). These minerals are great indicators of aqueous environments. In general, the formation of these minerals is due to processes involving hydrothermal fluids or sources (>100 °C). Some geological indications suggest that in the past there might have been a large amount of liquid water, which could have accumulated large reservoirs below the Martian surface. Thus, the laboratory study of Martian meteorites and interpretations of minerals present in these samples can contribute in a complementary way to the existing results of telescopic observations and/or missions of space probes as a strategy to indicate reservoirs of liquid water.

Strong seasonal and regional variations in the evaporation rate of liquid water on Mars

2021 ◽  
Author(s):  
Orkun Temel ◽  
Özgür Karatekin ◽  
Michael A. Mischna ◽  
Cem Berk Senel ◽  
Germán Martínez ◽  
...  
Keyword(s):  
Liquid Water ◽  
Evaporation Rate ◽  
Regional Variations ◽  
Water On Mars

Novel MEMS-Based Boiler Development for Low Temperature Applications

2009 ◽  
Author(s):  
K. Prather ◽  
H. Hemphill ◽  
I. Pjescic ◽  
C. Tranter ◽  
J. Dorton ◽  
...  
Keyword(s):  
Low Temperature ◽  
Evaporation Rate ◽  
Low Cost ◽  
Working Fluid ◽  
Heat Sources ◽  
Micro Fabrication ◽  
Capillary Action ◽  
Temperature Heat ◽  
Silicon Based ◽  
Temperature Applications

A novel MEMS-based boiler is fabricated and tested. The device is designed to operate from low-temperature heat sources using capillary action channels. The channels supply working fluid to the heated boiler surface, eliminating the need for traditional working fluid pumps. Two basic types of construction are evaluated. First, a more traditional silicon-based device is constructed and tested. Fabrication of the silicon boiler utilizes standard micro-fabrication practices. Second, a copper-based unit is fabricated and tested. Fabrication of the copper boiler focusses on low-cost techniques performed outside the scope of traditional micro-fab procedures. Results of these tests show the promise of non-traditional metals in low-temperature MEMS-based applications. The effectiveness of the copper boilers is shown to be 60% greater than their silicon counter parts. The copper-based prototypes exhibited a maximum evaporation rate for working fluid pumped across the boiling surface of 4.21 mg/sec.

scholarly journals Experimental Investigation of the Atmosphere-Regolith Water Cycle on Present-Day Mars

Sensors ◽  
2021 ◽  
Vol 21 (21) ◽  
pp. 7421
Author(s):  
Abhilash Vakkada Ramachandran ◽  
María-Paz Zorzano ◽  
Javier Martín-Torres
Keyword(s):  
Water Content ◽  
Triple Point ◽  
Liquid Water ◽  
Water Cycle ◽  
Pure Liquid ◽  
Martian Surface ◽  
Atmospheric Water ◽  
Near Surface ◽  
Martian Regolith

The water content of the upper layers of the surface of Mars is not yet quantified. Laboratory simulations are the only feasible way to investigate this in a controlled way on Earth, and then compare it with remote and in situ observations of spacecrafts on Mars. Describing the processes that may induce changes in the water content of the surface is critical to determine the present-day habitability of the Martian surface, to understand the atmospheric water cycle, and to estimate the efficiency of future water extraction procedures from the regolith for In Situ Resource Utilization (ISRU). This paper illustrates the application of the SpaceQ facility to simulate the near-surface water cycle under Martian conditions. Rover Environmental Monitoring Station (REMS) observations at Gale crater show a non-equilibrium situation in the atmospheric H2O volume mixing ratio (VMR) at night-time, and there is a decrease in the atmospheric water content by up to 15 g/m2 within a few hours. This reduction suggests that the ground may act at night as a cold sink scavenging atmospheric water. Here, we use an experimental approach to investigate the thermodynamic and kinetics of water exchange between the atmosphere, a non-porous surface (LN2-chilled metal), various salts, Martian regolith simulant, and mixtures of salts and simulant within an environment which is close to saturation. We have conducted three experiments: the stability of pure liquid water around the vicinity of the triple point is studied in experiment 1, as well as observing the interchange of water between the atmosphere and the salts when the surface is saturated; in experiment 2, the salts were mixed with Mojave Martian Simulant (MMS) to observe changes in the texture of the regolith caused by the interaction with hydrates and liquid brines, and to quantify the potential of the Martian regolith to absorb and retain water; and experiment 3 investigates the evaporation of pure liquid water away from the triple point temperature when both the air and ground are at the same temperature and the relative humidity is near saturation. We show experimentally that frost can form spontaneously on a surface when saturation is reached and that, when the temperature is above 273.15 K (0 °C), this frost can transform into liquid water, which can persist for up to 3.5 to 4.5 h at Martian surface conditions. For comparison, we study the behavior of certain deliquescent salts that exist on the Martian surface, which can increase their mass between 32% and 85% by absorption of atmospheric water within a few hours. A mixture of these salts in a 10% concentration with simulant produces an aggregated granular structure with a water gain of approximately 18- to 50-wt%. Up to 53% of the atmospheric water was captured by the simulated ground, as pure liquid water, hydrate, or brine.

scholarly journals Ice on Mars

1974 ◽  
Vol 13 (68) ◽  
pp. 173-185
Author(s):  
Robert P. Sharp
Keyword(s):  
Liquid Water ◽  
Polar Regions ◽  
Martian Surface ◽  
Ground Ice ◽  
Water Ice ◽  
Small Areas ◽  
Ice Caps ◽  
The North ◽  
Patterned Structures ◽  
Water Substance

Ice unquestionably exists on Mars. Annual polar-region frost blankets are principally solid CO2, and perennial residual ice caps near each pole are probably water ice, except for a part of the north polar cap which may consist of a 1 km thick mass of solid CO2. Minor amounts of carbon-dioxide clathrate (CO2 · ≈ 6H2O) presumably accompany the solid CO2. The annual frost blankets may have a concentric banding with an outermost very thin layer of water frost, an intermediate narrow zone of clathrate, and a major central core of solid CO2.Layered deposits and underlying homogeneous materials mantle large areas within both polar regions. These blankets are probably composed of dust, volcanic ash, or both, and possibly contain frozen volatiles. They may comprise the largest reservoir of water substance on the Martian surface.Ground ice formed by the freezing of ascending de-gassed water substance may underlie the surface of Mars. Localized collapse of small areas may be due to ground-ice deterioration, and recession of steep slopes may have been caused by ground-ice sapping.If liquid water ever existed in significant quantities on the Martian surface, intense frost shattering, widespread creep, and prolific development of patterned structures should have occurred because the thermal regimen of the surface is highly favorable to the freeze–thaw process. It is ineffective at present owing to the lack of liquid water.No evidence suggests that the residual ice caps have ever acted like terrestrial glaciers in terms of erosion and deposition. Currently, they are too thin, too cold, and presumably frozen to their substrates. Their most important function is to buffer the atmosphere in terms of its H2O and CO2 content, thereby exerting a modifying influence on the surface environment of the entire planet.

scholarly journals Identification of key parameters producing rainfall

MAUSAM ◽  
2021 ◽  
Vol 64 (2) ◽  
pp. 281-296
Author(s):  
RAJASRI SEN JAISWAL ◽  
V.S. NEELA ◽  
SONIA R. FREDRICK ◽  
M. RASHEED ◽  
LEENA ZAVERI ◽  
...  
Keyword(s):  
Satellite Data ◽  
Liquid Water ◽  
Tropical Rainfall Measuring Mission ◽  
Heat Energy ◽  
Cloud Liquid Water ◽  
Functional Relationships ◽  
Water Condensation ◽  
Surface Rainfall ◽  
Precipitation Water ◽  
Different Altitudes

o"kkZ ds eq[; izkpyksa dk irk yxkus ds fy, bl 'kks/k i= ls 'kks/kdrkZvksa us m".kdfVca/kh; o"kkZ ekiu fe’ku ¼Vh- vkj- ,e- ,e-½ mixzg vk¡dM+k vk/kkj dh tk¡p dh gSA bl rF; dks le>us ds mijkUr fd c<+us okys ok;q iklZy ds }kjk ikuh ds ok"ihdj.k] ok"i ds la?kuu vkSj m"ek ÅtkZ ds laogu ls es?k cursa gS vkSj o"kkZ gksrh gSA  'kks/kdrkZvksa us ok;qeaMy dh fofHkUu Å¡pkbZ;ksa ij o"kkZ izfØ;k ds eq[; lg;ksfx;ksa ds :i esa es?k nzo ty ¼lh-,y-MCY;w-½] o"kZ.k ty ¼ih-MCY;w-½ rFkk xqIr m"ek ¼,y-,p-½ ds ckjs esa tkudkjh izkIr djuh vkjaHk dj nh gSSA bu vk¡dM+ksa dks cgq lekJ;.k fun’kZ esa Mkyk x;k gSA ;g ik;k x;k gSS fd o"kkZ vkSj bu izkpyksa esa egRoiw.kZ lglaca/k gSA blls LFkkfir gq, dk;kZRed laca/kksa ls fdlh Hkh le; o"kkZ dk vkdyu fd;k tk ldrk gS c’krZs dkWyeuj lh-,y-MCY;w-] ih-MCY;w- vkSj ,y-,p- eku miyC?k gksaA ,d ;k nks ds LFkku ij bu lHkh rhuksa izkpyksa dks cgq lekJ;.k fun’kZ esa 'kkfey djus ds QyLo:i o"kkZ dk csgrj iwokZuqeku yxk;k tk ldk gSA lh- ,y- MCY;w-] ,y- ,p- vkSj ih- MCY;w- ds chp egRoiw.kZ lglaca/k gSaA In search of the key parameters causing rainfall, the authors have explored Tropical Rainfall Measuring Mission (TRMM) satellite data base. By realizing the fact that evaporation of water, condensation of vapour and transport of heat energy by a rising air parcel are all about formation of cloud and rain, the authors have started their quest considering cloud liquid water (CLW), precipitation water (PW) and latent heat (LH) at different altitudes of the atmosphere as major contributors to rainfall mechanism. These data have been fitted to multiple regressions. It is found that significant correlations exist between rainfall and these parameters. The functional relationships so established are able to estimate surface rainfall at any instant, provided columnar CLW, PW and LH values are available. Inclusion of all the three parameters in multiple regression leads to better predictability of rainfall, instead of one or two. Significant correlations exist between CLW, LH and PW.

scholarly journals Paradox of Flows on Mars

2005 ◽  
Vol 13 ◽  
pp. 918-920
Author(s):  
L.V. Ksanfomality
Keyword(s):  
High Resolution ◽  
Liquid Water ◽  
Martian Surface ◽  
Mars Global Surveyor ◽  
High Resolution Images ◽  
Unknown Objects

Using the high-resolution images acquired by cameras onboard the MARS GLOBAL SURVEYOR orbiter made it possible to reveal the previously unknown objects on the Martian surface, which changed dramatically a notion of Mars as a dry, hydrologically dead planet (Malin and Edgett, 2000). Examination of new images shows that the nature of some extended dark formations on the slopes of craters and uplands may be associated with contemporary abundant sources of liquid water arising on the slopes at small depths below the level of surrounding plains.

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