Climate of Mars

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Further information: Atmosphere of Mars
Mosaic image of Mars as seen by Viking 1, February 22, 1980

The climate of Mars has been an issue of scientific curiosity for centuries, not least because Mars is the only terrestrial planet whose surface can be directly observed in detail from the Earth with help from a telescope.

Although Mars is smaller at 11% of Earth's mass and 50% farther from the Sun than the Earth, its climate has important similarities, such as the polar ice caps, seasonal changes and the observable presence of weather patterns. It has attracted sustained study from planetologists and climatologists. Although Mars's climate has similarities to Earth's, including seasons and periodic ice ages, there are also important differences such as the absence of liquid water (though frozen water exists) and much lower thermal inertia. Mars' atmosphere has a scale height of approximately 11 km (36,000 ft), 60% greater than that on Earth. The climate is of considerable relevance to the question of whether life is or was present on the planet. The climate briefly received more interest in the news due to NASA measurements indicating increased sublimation of the south polar icecap leading to some popular press speculation that Mars was undergoing a parallel bout of global warming,[1] though global average temperature has actually cooled in recent decades.

Mars has been studied by Earth-based instruments since as early as the 17th century but it is only since the exploration of Mars began in the mid-1960s that close-range observation has been possible. Flyby and orbital spacecraft have provided data from above, while direct measurements of atmospheric conditions have been provided by a number of landers and rovers. Advanced Earth orbital instruments today continue to provide some useful "big picture" observations of relatively large weather phenomena.

The first Martian flyby mission was Mariner 4 which arrived in 1965. That quick two day pass (July 14–15, 1965) was limited and crude in terms of its contribution to the state of knowledge of Martian climate. Later Mariner missions (Mariner 6, and Mariner 7) filled in some of the gaps in basic climate information. Data based climate studies started in earnest with the Viking program in 1975 and continues with such probes as the Mars Reconnaissance Orbiter.

This observational work has been complemented by a type of scientific computer simulation called the Mars General Circulation Model.[2] Several different iterations of MGCM have led to an increased understanding of Mars as well as the limits of such models. Models are limited in their ability to represent atmospheric physics that occurs at a smaller scale than their resolution. They also may be based on inaccurate or unrealistic assumptions about how Mars works and certainly suffer from the quality and limited density in time and space of climate data from Mars.

Historical climate observations[edit]

Giancomo Miraldi determined in 1704 that the southern cap is not centered on the rotational pole of Mars.[3] During the opposition of 1719, Miraldi observed both polar caps and temporal variability in their extent.

William Herschel was the first to deduce the low density of the Martian atmosphere in his 1784 paper entitled On the remarkable appearances at the polar regions on the planet Mars, the inclination of its axis, the position of its poles, and its spheroidal figure; with a few hints relating to its real diameter and atmosphere. When two faint stars passed close to Mars with no effect on their brightness, Herschel correctly concluded that this meant that there was little atmosphere around Mars to interfere with their light.[3]

Honore Flaugergues 1809 discovery of "yellow clouds" on the surface of Mars is the first known observation of Martian dust storms.[4] Flaugergues also observed in 1813 significant polar ice waning during Martian springtime. His speculation that this meant that Mars was warmer than earth proved inaccurate.

Martian paleoclimatology[edit]

Prior to any serious examination of Martian paleoclimatology one has to agree on terms, especially broad terms of planetary ages. There are two dating systems now in use for Martian geological time. One is based on crater density and has three ages: Noachian, Hesperian, and Amazonian. The other is a mineralogical timeline, also having three ages: Phyllocian, Theikian, and Siderikian.

Recent observations and modeling are producing information not only about the present climate and atmospheric conditions on Mars but also about its past. The Noachian-era Martian atmosphere had long been theorized to be carbon dioxide rich. Recent spectral observations of deposits of clay minerals on Mars and modeling of clay mineral formation conditions[5] have found that there is little to no carbonate present in clay of that era. Clay formation in a carbon dioxide rich environment is always accompanied by carbonate formation, though the carbonate may later be dissolved by volcanic acidity.

The discovery of water-formed minerals on Mars, including hematite and jarosite, by the Opportunity rover and goethite by the Spirit rover, has led to the conclusion that climatic conditions in the distant past allowed for free-flowing water on Mars. The morphology of some crater impacts on Mars indicate that the ground was wet at the time of impact.[6] Geomorphic observations of both landscape erosion rates[7] and Martian valley networks[8] also strongly imply warmer, wetter conditions on Noachian-era Mars (earlier than about 4 billion years ago). However, chemical analysis of Martian meteorite samples suggests that the ambient near-surface temperature of Mars has most likely been below 0 °C for the last four billion years.[9]

Some scientists maintain that the great mass of the Tharsis volcanoes has had a major influence on the climate of Mars. Erupting volcanoes give off great amounts of gas, mainly water vapor and CO2. Enough gas may have been released by volcanoes to have made the earlier Martian atmosphere thicker than Earth's. The volcanoes could also have emitted enough H2O to cover the whole Martian surface to a depth of 120 m (390 ft). CO2 is a greenhouse gas that raises the temperature of a planet: it traps heat by absorbing infrared radiation. So Tharsis volcanoes, by giving off CO2, could have made Mars more Earth-like in the past. Mars may have once had a much thicker and warmer atmosphere, and oceans and/or lakes may have been present.[10] It has, however, proven extremely difficult to construct convincing global climate models for Mars which produce temperatures above 0 °C at any point in its history,[11] though this may simply reflect problems in accurately calibrating such models.

Weather[edit]

Martian Morning Clouds - Viking Orbiter 1 (taken in 1976) - (February 12, 2014).

Mars' temperature and circulation vary from year to year (as expected for any planet with an atmosphere). Mars lacks oceans, a source of much inter-annual variation on Earth.[clarification needed] Mars Orbiter Camera data beginning in March 1999 and covering 2.5 Martian years[12] show that Martian weather tends to be more repeatable and hence more predictable than that of Earth. If an event occurs at a particular time of year in one year, the available data (sparse as it is) indicate that it is fairly likely to repeat the next year at nearly the same location give or take a week.

On September 29, 2008, the Phoenix lander took pictures of snow falling from clouds 4.5 km above its landing site near Heimdall crater. The precipitation vaporized before reaching the ground, a phenomenon called virga.[13]

Clouds[edit]

Animation of ice clouds moving above the Phoenix landing site over a period of ten minutes (August 29, 2008).

Mars' dust storms can kick up fine particles in the atmosphere around which clouds can form. These clouds can form very high up, up to 100 km (62 mi) above the planet.[14] The clouds are very faint and can only be seen reflecting sunlight against the darkness of the night sky. In that respect, they look similar to the mesospheric clouds, also known as noctilucent clouds on Earth, which occur about 80 km (50 mi) above our planet.

Temperature[edit]

Martian temperatures have been measured by various means:

Early flyby probes (Mariner 4) and later orbiters used radio occultation to perform aeronomy. With chemical composition already deduced from spectroscopy, temperature and pressure could then be derived. Nevertheless, flyby occultations can only measure properties along two transects, at their trajectories' entries and exits from Mars' disk as seen from Earth. This results in weather "snapshots" at a particular area, at a particular time. Orbiters then increase the number of radio transects.

Later missions, starting with the dual Mariner 6 and 7 flybys, plus the Soviet Mars 2 and 3, carried infrared detectors to measure radiant energy. Mariner 9 was the first to place an infrared radiometer and spectrometer in Mars orbit in 1971, along with its other instruments and radio transmitter. Viking 1 and 2 followed, with not merely Infrared Thermal Mappers (IRTM).[15] The missions could also corroborate these remote sensing datasets with not only their in situ lander metrology booms,[16] but with higher-altitude temperature and pressure sensors for their descent.[17]

Differing in situ values have been reported for the average temperature on Mars,[18] with a common value being −55 °C (218 K; −67 °F).[19] Surface temperatures may reach a high of about 20 °C (293 K; 68 °F) at noon, at the equator, and a low of about −153 °C (120 K; −243 °F) at the poles.[20] Actual temperature measurements at the Viking landers' site range from −17.2 °C (256.0 K; 1.0 °F) to −107 °C (166 K; −161 °F). The warmest soil temperature on the Mars surface estimated by the Viking Orbiter was 27 °C (300 K; 81 °F).[21] The Spirit rover recorded a maximum daytime air temperature in the shade of 35 °C (308 K; 95 °F), and regularly recorded temperatures well above 0 °C (273 K; 32 °F), except in winter.[22]

It has been reported that "On the basis of the nightime air temperature data, every northern spring and early northern summer yet observed were identical to within the level of experimental error (to within ±1 °C)" but that the "daytime data, however, suggest a somewhat different story, with temperatures varying from year-to-year by up to 6 °C in this season.[23] This day-night discrepancy is unexpected and not understood". In southern spring and summer, variance is dominated by dust storms which increase the value of the night low temperature and decrease the daytime peak temperature.[24] This results in a small (20 °C) decrease in average surface temperature, and a moderate (30 °C) increase in upper atmosphere temperature.[25]

Before and after the Viking missions, Martian temperatures were determined from Earth via microwave spectroscopy. As the microwave beam, of under 1 arcminute, is larger than the disk of the planet, the results are global averages.[26] Later, the Mars Global Surveyor's Thermal Emission Spectrometer and to a lesser extent 2001 Mars Odyssey's THEMIS could not merely reproduce infrared measurements but intercompare lander, rover, and Earth microwave data. The Mars Reconnaissance Orbiter's Mars Climate Sounder can similarly derive atmospheric profiles.

The datasets "suggest generally colder atmospheric temperatures and lower dust loading in recent decades on Mars than during the Viking Mission,"[27] though Viking data had previously been revised downward.[28] The TES data indicates "Much colder (10-20 K) global atmospheric temperatures were observed during the 1997 versus 1977 perihelion periods" and "that the global aphelion atmosphere of Mars is colder, less dusty, and cloudier than indicated by the established Viking climatology," again, taking into account the Wilson and Richardson revisions to Viking data.[29]

A later comparison, while admitting "it is the microwave record of air temperatures which is the most representative," attempted to merge the discontinuous spacecraft record. No measurable trend in global average temperature between Viking IRTM and MGS TES was visible. "Viking and MGS air temperatures are essentially indistinguishable for this period, suggesting that the Viking and MGS eras are characterized by essentially the same climatic state." It found "a strong dichotomy" between the northern and southern hemispheres, a "very asymmetric paradigm for the Martian annual cycle: a northern spring and summer which is relatively cool, not very dusty, and relatively rich in water vapor and ice clouds; and a southern summer rather similar to that observed by Viking with warmer air temperatures, less water vapor and water ice, and higher levels of atmospheric dust."[30]

Atmospheric properties and processes[edit]

Low atmospheric pressure[edit]

The Martian atmosphere is composed mainly of carbon dioxide and has a mean surface pressure of about 600 pascals (Pa), much lower than the Earth's 101,000 Pa. One effect of this is that Mars' atmosphere can react much more quickly to a given energy input than that of Earth's atmosphere.[31] As a consequence, Mars is subject to strong thermal tides produced by solar heating rather than a gravitational influence. These tides can be significant, being up to 10% of the total atmospheric pressure (typically about 50 Pa). Earth's atmosphere experiences similar diurnal and semidiurnal tides but their effect is less noticeable because of Earth's much greater atmospheric mass.

Although the temperature on Mars can reach above freezing (0 °C (273 K; 32 °F)), liquid water is unstable over much of the planet, as the atmospheric pressure is below water's triple point and water ice sublimes into water vapor. Exceptions to this are the low-lying areas of the planet, most notably in the Hellas Planitia impact basin, the largest such crater on Mars. It is so deep that the atmospheric pressure at the bottom reaches 1155 Pa, which is above the triple point, so if the temperature exceeded 0 °C liquid water could exist there.[citation needed]

Wind[edit]

Curiosity rover's parachute flapping in the Martian wind (HiRISE/MRO) (August 12, 2012 to January 13, 2013).

The surface of Mars has a very low thermal inertia, which means it heats quickly when the sun shines on it. Typical daily temperature swings, away from the polar regions, are around 100 K. On Earth, winds often develop in areas where thermal inertia changes suddenly, such as from sea to land. There are no seas on Mars, but there are areas where the thermal inertia of the soil changes, leading to morning and evening winds akin to the sea breezes on Earth.[32] The Antares project "Mars Small-Scale Weather" (MSW) has recently identified some minor weaknesses in current global climate models (GCMs) due to the GCMs' more primitive soil modeling "heat admission to the ground and back is quite important in Mars, so soil schemes have to be quite accurate. "[33] Those weaknesses are being corrected and should lead to more accurate future assessments, but make continued reliance on older predictions of modeled Martian climate somewhat problematic.

At low latitudes the Hadley circulation dominates, and is essentially the same as the process which on Earth generates the trade winds. At higher latitudes a series of high and low pressure areas, called baroclinic pressure waves, dominate the weather. Mars is dryer and colder than Earth, and in consequence dust raised by these winds tends to remain in the atmosphere longer than on Earth as there is no precipitation to wash it out (excepting CO2 snowfall).[34] One such cyclonic storm was recently captured by the Hubble space telescope (pictured below).

One of the major differences between Mars' and Earth's Hadley circulations is their speed[35] which is measured on an overturning timescale. The overturning timescale on Mars is about 100 Martian days while on Earth, it is over a year.

Effect of dust storms[edit]

2001 Hellas Basin dust storm
Time-lapse composite of Martian horizon during Sols 1205 (0.94), 1220 (2.9), 1225 (4.1), 1233 (3.8), 1235 (4.7) shows how much sunlight the July 2007 dust storms blocked; Tau of 4.7 indicates 99% blocked.

Dust Storm on Mars.

November 18, 2012
November 25, 2012
Locations of Opportunity and Curiosity rovers are noted (MRO).

When the Mariner 9 probe arrived at Mars in 1971, the world expected to see crisp new pictures of surface detail. Instead they saw a near planet-wide dust storm[36] with only the giant volcano Olympus Mons showing above the haze. The storm lasted for a month, an occurrence scientists have since learned is quite common on Mars.

As observed by the Viking spacecraft from the surface,[24] "during a global dust storm the diurnal temperature range narrowed sharply, from fifty degrees to only about ten degrees, and the wind speeds picked up considerably—indeed, within only an hour of the storm's arrival they had increased to 17 m/s (61 km/h), with gusts up to 26 m/s (94 km/h). Nevertheless, no actual transport of material was observed at either site, only a gradual brightening and loss of contrast of the surface material as dust settled onto it." On June 26, 2001, the Hubble Space Telescope spotted a dust storm brewing in Hellas Basin on Mars (pictured right). A day later the storm "exploded" and became a global event. Orbital measurements showed that this dust storm reduced the average temperature of the surface and raised the temperature of the atmosphere of Mars by 30 °C.[25] The low density of the Martian atmosphere means that winds of 18 to 22 m/s (65 to 79 km/h) are needed to lift dust from the surface, but since Mars is so dry, the dust can stay in the atmosphere far longer than on Earth, where it is soon washed out by rain. The season following that dust storm had daytime temperatures 4 °C below average. This was attributed to the global covering of light-colored dust that settled out of the dust storm, temporarily increasing Mars' albedo.[37]

In mid-2007 a planet-wide dust storm posed a serious threat to the solar-powered Spirit and Opportunity Mars Exploration Rovers by reducing the amount of energy provided by the solar panels and necessitating the shut-down of most science experiments while waiting for the storms to clear.[38] Following the dust storms, the rovers had significantly reduced power due to settling of dust on the arrays.

Dust storms are most common during perihelion, when the planet receives 40 percent more sunlight than during aphelion. During aphelion water ice clouds form in the atmosphere, interacting with the dust particles and affecting the temperature of the planet.[39]

It has been suggested that dust storms on Mars could play a role in storm formation similar to that of water clouds on Earth.[citation needed] Observation since the 1950s has shown that the chances of a planet-wide dust storm in a particular Martian year are approximately one in three.[40]

Saltation[edit]

The process of geological saltation is quite important on Mars as a mechanism for adding particulates to the atmosphere. Saltating sand particles have been observed on the MER Spirit rover.[41] Theory and real world observations have not agreed with each other, classical theory missing up to half of real-world saltating particles.[42] A new model more closely in accord with real world observations demonstrates that saltating particles create an electrical field that increases the saltation effect. Mars grains saltate in 100 times higher and longer trajectories and reach 5-10 times higher velocities than Earth grains do.[43]

Repeating northern annular cloud[edit]

Hubble view of the colossal polar cloud on Mars

A large doughnut shaped cloud appears in North polar region of Mars around the same time every Martian year and of about the same size.[44] It forms in the morning, dissipates by the Martian afternoon.[44] The outer diameter of the cloud is roughly 1,600 km (1,000 mi), and the inner hole or eye is 320 km (200 mi) across.[45] The cloud is thought to be composed of water-ice,[45] so it is white in color, unlike the more common dust storms.

It looks like a cyclonic storm, similar to a hurricane, but it does not rotate.[44] The cloud appears during the northern summer and at high latitude. Speculation is that this is due to unique climate conditions near the northern pole.[45] Cyclone-like storms were first detected during the Viking orbital mapping program, but the northern annular cloud is nearly three times larger.[45] The cloud has also been detected by various probes and telescopes including the Hubble and Mars Global Surveyor.[44][45]

Other repeating events are dust storms and dust devils.[45]

Methane presence[edit]

Methane map

Although methane is a greenhouse gas on Earth, the small amounts that have been claimed to be present on Mars would have little effect on the Martian global climate. Trace amounts of methane (CH4) at concentration of several parts per billion (ppb), were first reported in the atmosphere of Mars by a team at the NASA Goddard Space Flight Center in 2003.[46][47]

Methane on Mars - "potential sources and sinks" (November 2, 2012).

In March 2004 the Mars Express Orbiter[48][49][50][51] and ground based observations from Canada-France-Hawaii Telescope[52] also suggested the presence of methane in the atmosphere with a mole fraction of about 10 nmol/mol.[51] However, the complexity of these observations has sparked discussion as to the reliability of the results.[53]

Since breakup of that much methane by ultraviolet light would only take 350 years under current Martian conditions, if methane is present some sort of active source must be replenishing the gas.[54] Clathrate hydrates,[55] or water-rock reactions [56] could be possible geological sources of methane but there is presently no consensus on the source or existence of Martian methane.

The Curiosity rover landed on Mars in August 2012. It is able to make precise abundance measurements and also distinguish between different isotopologues of methane.[57] The first measurements with the Tunable Laser Spectrometer (TLS) indicate that there is less than 5 ppb of methane at the landing site.[58][59][60][61] On September 19, 2013 NASA scientists used further measurements from Curiosity to report a non-detection of atmospheric methane with a measured value of 0.18±0.67 ppbv corresponding to an upper limit of 1.3 ppbv (95% confidence limit).[62]

The Indian Mars Orbiter Mission, launched in November 5, 2013, will attempt to detect and map the sources of methane, if they exist.[63] The ExoMars Trace Gas Orbiter planned to launch in 2016 would further study the methane,[64][65] as well as its decomposition products such as formaldehyde and methanol.

Carbon dioxide carving[edit]

Mars Reconnaissance Orbiter images suggest an unusual erosion effect occurs based on Mars' unique climate. Spring warming in certain areas leads to CO2 ice subliming and flowing upwards, creating highly unusual erosion patterns called "spider gullies".[66] Translucent CO2 ice forms over winter and as the spring sunlight warms the surface, it vaporizes the CO2 to gas which flows uphill under the translucent CO2 ice. Weak points in that ice lead to CO2 geysers.[66]

Mountains[edit]

Planet Marsvolatile gases – (Curiosity rover, October 2012).

Martian storms are significantly affected by Mars' large mountain ranges.[67] Individual mountains like record holding Olympus Mons (27 km (89,000 ft)) can affect local weather but larger weather effects are due to the larger collection of volcanoes in the Tharsis region.

One unique repeated weather phenomena involving Mountains is a spiral dust cloud that forms over Arsia Mons. The spiral dust cloud over Arsia Mons can tower 15 to 30 km (49,000 to 98,000 ft) above the volcano.[68] Clouds are present around Arsia Mons throughout the Martian year, peaking in late summer.[69]

Clouds surrounding mountains display a seasonal variability. Clouds at Olympus Mons and Ascreaus Mons appear in northern hemisphere spring and summer, reaching a total maximum area of approximately 900,000 km2 and 1,000,000 km2 respectively in late spring. Clouds around Alba Patera and Pavonis Mons show an additional, smaller peak in late summer. Very few clouds were observed in winter. Predictions from the Mars General Circulation Model are consistent with these observations.[69]

Polar caps[edit]

An illustration of what Mars might have looked like during an ice age between 2.1 million and 400,000 years ago, when Mars's axial tilt is believed to have been much larger than today.
HiRISE image of "dark dune spots" and fans formed by eruptions of CO2 gas geysers on Mars' south polar ice sheet.

Mars has ice caps at its north pole and south pole, which mainly consist of water ice; however, there is frozen carbon dioxide (dry ice) present on their surfaces. Dry ice accumulates in the north polar region (Planum Boreum) in winter only, subliming completely in summer, while the south polar region additionally has a permanent dry ice cover up to eight meters (25 feet) thick.[70] This difference is due to the higher elevation of the south pole.

So much of the atmosphere can condense at the winter pole that the atmospheric pressure can vary by up to a third of its mean value. This condensation and evaporation will cause the proportion of the noncondensable gases in the atmosphere to change inversely.[34] The eccentricity of Mars's orbit affects this cycle, as well as other factors. In the spring and autumn wind due to the carbon dioxide sublimation process is so strong that it can be a cause of the global dust storms mentioned above.[71]

The northern polar cap has a diameter of approximately 1,000 km during the northern Mars summer,[72] and contains about 1.6 million cubic kilometres of ice, which if spread evenly on the cap would be 2 km thick.[73] (This compares to a volume of 2.85 million cubic kilometres for the Greenland ice sheet.) The southern polar cap has a diameter of 350 km and a maximum thickness of 3 km.[74] Both polar caps show spiral troughs, which were formerly believed to form as a result of differential solar heating, coupled with the sublimation of ice and condensation of water vapor.[75][76] Recent analysis of ice penetrating radar data from SHARAD has demonstrated that the spiral troughs are formed from a unique situation in which high density katabatic winds descend from the polar high to transport ice and create large wavelength bedforms.[77][78] The spiral shape comes from Coriolis effect forcing of the winds, much like winds on earth spiral to form a hurricane. The troughs did not form with either ice cap, instead they began to form between 2.4 million and 500,000 years ago, after three fourths of the ice cap was in place. This suggests that a climatic shift allowed for their onset. Both polar caps shrink and regrow following the temperature fluctuation of the Martian seasons; there are also longer-term trends that are not fully understood.

During the southern hemisphere spring, solar heating of dry ice deposits at the south pole leads in places to accumulation of pressurized CO2 gas below the surface of the semitransparent ice, warmed by absorption of radiation by the darker substrate. After attaining the necessary pressure, the gas bursts through the ice in geyser-like plumes. While the eruptions have not been directly observed, they leave evidence in the form of "dark dune spots" and lighter fans atop the ice, representing sand and dust carried aloft by the eruptions, and a spider-like pattern of grooves created below the ice by the outrushing gas.[79][80] (see Geysers on Mars.) Eruptions of nitrogen gas observed by Voyager 2 on Triton are thought to occur by a similar mechanism.

Solar wind[edit]

Mars lost most of its magnetic field about four billion years ago. As a result, solar wind and cosmic radiation interacts directly with the Martian ionosphere. This keeps the atmosphere thinner than it would otherwise be by solar wind action constantly stripping away atoms from the outer atmospheric layer.[81] Most of the historical atmospheric loss on Mars can be traced back to this solar wind effect. Current theory posits a weakening solar wind and thus today's atmosphere stripping effects are much less than those in the past when the solar wind was stronger.[citation needed]

Seasons[edit]

In spring, sublimation of ice causes sand from below the ice layer to form fan-shaped deposits on top of the seasonal ice.

Mars has an axial tilt of 25.2°. This means that there are seasons on Mars, just as on Earth. The eccentricity of Mars' orbit is 0.1, much greater than the Earth's present orbital eccentricity of about 0.02. The large eccentricity causes the insolation on Mars to vary as the planet orbits the Sun (the Martian year lasts 687 days, roughly 2 Earth years). As on Earth, Mars' obliquity dominates the seasons but, because of the large eccentricity, winters in the southern hemisphere are long and cold while those in the North are short and warm.

It is now widely believed that ice accumulated when Mars' orbital tilt was very different from what it is now (the axis the planet spins on has considerable "wobble," meaning its angle changes over time).[82][83][84] A few million years ago, the tilt of the axis of Mars was 45 degrees instead of its present 25 degrees. Its tilt, also called obliquity, varies greatly because its two tiny moons cannot stabilize it like our moon.

Many features on Mars, especially in the Ismenius Lacus quadrangle, are believed to contain large amounts of ice. The most popular model for the origin of the ice is climate change from large changes in the tilt of the planet's rotational axis. At times the tilt has even been greater than 80 degrees[85][86] Large changes in the tilt explains many ice-rich features on Mars.

Studies have shown that when the tilt of Mars reaches 45 degrees from its current 25 degrees, ice is no longer stable at the poles.[87] Furthermore, at this high tilt, stores of solid carbon dioxide (dry ice) sublimate, thereby increasing the atmospheric pressure. This increased pressure allows more dust to be held in the atmosphere. Moisture in the atmosphere will fall as snow or as ice frozen onto dust grains. Calculations suggest this material will concentrate in the mid-latitudes.[88][89] General circulation models of the Martian atmosphere predict accumulations of ice-rich dust in the same areas where ice-rich features are found.[90] When the tilt begins to return to lower values, the ice sublimates (turns directly to a gas) and leaves behind a lag of dust.[91][91][92] The lag deposit caps the underlying material so with each cycle of high tilt levels, some ice-rich mantle remains behind.[93] Note, that the smooth surface mantle layer probably represents only relative recent material.

The seasons present unequal lengths are as follows:

Season Sols
(on Mars)
Days
(on Earth)
Northern Spring, Southern Autumn: 193.30 92.764
Northern Summer, Southern Winter: 178.64 93.647
Northern Autumn, Southern Spring: 142.70 89.836
Northern Winter, Southern Summer: 153.95 88.997

Precession in the alignment of the obliquity and eccentricity lead to global warming and cooling ('great' summers and winters) with a period of 170,000 years.[94]

Like Earth, the obliquity of Mars undergoes periodic changes which can lead to long-lasting changes in climate. Once again, the effect is more pronounced on Mars because it lacks the stabilizing influence of a large moon. As a result the obliquity can alter by as much as 45°. Jacques Laskar, of France's National Centre for Scientific Research, argues that the effects of these periodic climate changes can be seen in the layered nature of the ice cap at the Martian north pole.[95] Current research suggests that Mars is in a warm interglacial period which has lasted more than 100,000 years.[96]

Because the Mars Global Surveyor was able to observe Mars for 4 Martian years, it was found that Martian weather was similar from year to year. Any differences were directly related to changes in the solar energy that reached Mars. Scientists were even able to accurately predict dust storms that would occur during the landing of Beagle 2. Regional dust storms were discovered to be closely related to where dust was available.[97]

Evidence for recent climatic change[edit]

Pits in south polar ice cap, MGS 1999, NASA

There have been regional changes around the south pole (Planum Australe) over the past few Martian years. In 1999 the Mars Global Surveyor photographed pits in the layer of frozen carbon dioxide at the Martian south pole. Because of their striking shape and orientation these pits have become known as swiss cheese features. In 2001 the craft photographed the same pits again and found that they had grown larger, retreating about 3 meters in one Martian year.[98] These features are caused by the sublimation of the dry ice layer, thereby exposing the inert water ice layer. More recent observations indicate that the ice at Mars' south pole is continuing to sublime.[99] The pits in the ice continue to grow by about 3 meters per Martian year. Malin states that conditions on Mars are not currently conducive to the formation of new ice. A NASA press release has suggested that this indicates a "climate change in progress"[100] on Mars. In a summary of observations with the Mars Orbiter Camera, researchers speculated that some dry ice may have been deposited between the Mariner 9 and the Mars Global Surveyor mission. Based on the current rate of loss, the deposits of today may be gone in a hundred years.[97]

Elsewhere on the planet, low latitude areas have more water ice than they should have given current climatic conditions.[101] Mars Odyssey "is giving us indications of recent global climate change in Mars," said Jeffrey Plaut, project scientist for the mission at NASA's Jet Propulsion Laboratory, in non-peer reviewed published work in 2003.

Attribution theories[edit]

Polar changes[edit]

Colaprete et al. conducted simulations with the Mars General Circulation Model which show that the local climate around the Martian south pole may currently be in an unstable period. The simulated instability is rooted in the geography of the region, leading the authors to speculate that the sublimation of the polar ice is a local phenomenon rather than a global one.[102] The researchers showed that even with a constant solar luminosity the poles were capable of jumping between states of depositing or losing ice. The trigger for a change of states could be either increased dust loading in the atmosphere or an albedo change due to deposition of water ice on the polar cap.[103] This theory is somewhat problematic due to the lack of ice depositation after the 2001 global dust storm.[37] Another issue is that the accuracy of the Mars General Circulation Model decreases as the scale of the phenomenon becomes more local.

It has been argued that "observed regional changes in south polar ice cover are almost certainly due to a regional climate transition, not a global phenomenon, and are demonstrably unrelated to external forcing."[94] Writing in a Nature news story, Chief News and Features Editor Oliver Morton said "The warming of other solar bodies has been seized upon by climate sceptics. On Mars, the warming seems to be down to dust blowing around and uncovering big patches of black basaltic rock that heat up in the day."[37][104]

Solar irradiance[edit]

K. I. Abdusamatov has proposed that "parallel global warmings" observed simultaneously on Mars and on Earth can only be a consequence of the same factor: a long-time change in solar irradiance."[105] While some individuals who reject the science of global warming take this as proof that humans are not causing climate change,[106] Abdusamatov's hypothesis has not been accepted by the scientific community. His assertions have not been published in the peer-reviewed literature, and have been dismissed by other scientists, who have stated that "the idea just isn't supported by the theory or by the observations" and that it "doesn't make physical sense."[107] Other scientists have proposed that the observed variations are caused by irregularities in the orbit of Mars or a possible combination of solar and orbital effects.[108]

Mars Global Climate Zones, based on temperature, modified by topography, albedo, actual solar radiation.

Climate zones[edit]

Terrestrial Climate zones first have been defined by Wladimir Köppen based on the distribution of vegetation groups. Climate classification is furthermore based on temperature, rainfall, and subdivided based upon differences in the seasonal distribution of temperature and precipitation; and a separate group exists for extrazonal climates like in high altitudes. Mars has neither vegetation nor rainfall, so any climate classification could be only based upon temperature; a further refinement of the system may be based on dust distribution, water vapor content, occurrence of snow. Solar Climate Zones can also be easily defined for Mars.[109]

Current missions[edit]

The 2001 Mars Odyssey is currently orbiting Mars and taking global atmospheric temperature measurements with the TES instrument. The Mars Reconnaissance Orbiter is currently taking daily weather and climate related observations from orbit. One of its instruments, the Mars climate sounder is specialized for climate observation work. The MSL was launched in November 2011 and landed on Mars on August 6, 2012.[110]

Curiosity roverTemperature, Pressure, Humidity at Gale Crater on Mars (August 2012 – February 2013).

Future missions[edit]

See also[edit]

References[edit]

  1. ^ Francis Reddy (September 23, 2005). "MGS sees changing face of Mars". Astronomy Magazine. Retrieved September 6, 2007. 
  2. ^ NASA. "Mars General Circulation Modeling". NASA. Retrieved February 22, 2007. 
  3. ^ a b Exploring Mars in the 1700s
  4. ^ Exploring Mars in the 1800s
  5. ^ "Clay studies might alter Mars theories". Science Daily. July 19, 2007. Archived from the original on September 30, 2007. Retrieved September 6, 2007. 
  6. ^ Carr, M.H., et al. (1977), Martian impact craters and emplacement of ejecta by surface flow, J. Geophys. Res., 82, 4055-65.
  7. ^ Golombek, M.P., and Bridges, N.T. (2000), Erosion rates on Mars and implications for climate change: constraints from the Pathfinder landing site, J. Geophys. Res., 105(E1), 1841–1853
  8. ^ Craddock, R.A., and Howard, A.D. (2002), The case for rainfall on a warm, wet early Mars, J. Geophys. Res., 107(E11), doi:10.1029/2001JE001505
  9. ^ Shuster, David L.; Weiss, Benjamin P. (July 22, 2005). "Martian Surface Paleotemperatures from Thermochronology of Meteorites". Science 309 (5734): 594–600. Bibcode:2005Sci...309..594S. doi:10.1126/science.1113077. PMID 16040703. 
  10. ^ Hartmann, W. 2003. A Traveler's Guide to Mars. Workman Publishing. NY NY.
  11. ^ aberle, R.M. (1998), Early Climate Models, J. Geophys. Res., 103(E12),28467-79
  12. ^ "Weather at the Mars Exploration Rover and Beagle 2 Landing Sites". Malin Space Science Systems. Retrieved September 8, 2007. 
  13. ^ "NASA Mars Lander Sees Falling Snow, Soil Data Suggest Liquid Past". September 29, 2008. Retrieved October 3, 2008. 
  14. ^ Mars Clouds Higher Than Any On Earth
  15. ^ "National Space Science Data Center: Infrared Thermal Mapper (IRTM)". Retrieved September 14, 2014. 
  16. ^ "National Space Science Data Center: Meteorology". Retrieved September 14, 2014. 
  17. ^ "National Space Science Data Center: Atmospheric Structure". Retrieved September 14, 2014. 
  18. ^ Eydelman, Albert (2001). "Temperature on the Surface of Mars". The Physics Factbook. 
  19. ^ "Focus Sections :: The Planet Mars". MarsNews.com. Retrieved September 8, 2007. 
  20. ^ "Mars Facts". NASA. Retrieved June 20, 2013. 
  21. ^ James E. Tillman Mars – Temperature Overview
  22. ^ Extreme Planet Takes its Toll Jet Propulsion Laboratory Featured Story, June 12, 2007.
  23. ^ Liu, Junjun; Mark I. Richardson; R. J. Wilson (15 August 2003). "An assessment of the global, seasonal, and interannual spacecraft record of Martian climate in the thermal infrared" (– Scholar search). Journal of Geophysical Research 108 (5089): 5089. Bibcode:2003JGRE..108.5089L. doi:10.1029/2002JE001921. Retrieved September 8, 2007. [dead link]
  24. ^ a b William Sheehan, The Planet Mars: A History of Observation and Discovery, Chapter 13 (available on the web)
  25. ^ a b Mark A. Gurwell, Edwin A. Bergin, Gary J. Melnick and Volker Tolls, "Mars surface and atmospheric temperature during the 2001 global dust storm," Icarus, Volume 175, Issue 1, May 2005, Pages 23-3, doi:10.1016/j.icarus.2004.10.009
  26. ^ Clancy, R. (August 30, 1990). "Global Changes in the 0-70 km Thermal Structure of the Mars Atmosphere Derived from 1975 to 1989 Microwave CO Spectra". Journal of Geophysical Research 95 (9): 14,543–14,554. 
  27. ^ Bell, J et al. (August 28, 2009). "Mars Reconnaissance Orbiter Mars Color Imager (MARCI): Instrument Description, Calibration, and Performance". Journal of Geophysical Research 114 (8). 
  28. ^ Wilson, R.; Richardson, M. (2000). "The Martian Atmosphere During the Viking I Mission, I: Infrared Measurements of Atmospheric Temperatures Revisited". Icarus 145: 555–579. 
  29. ^ Clancy, R. (April 25, 2000). "An intercomparison of ground-based millimeter, MGS TES, and Viking atmospheric temperature measurements: Seasonal and interannual variability of temperatures and dust loading in the global Mars atmosphere". Journal of Geophysical Research 105 (4): 9553–9571. 
  30. ^ Liu, J., Richardson, M. (August 2003). "An assessment of the global, seasonal, and interannual spacecraft record of Martian climate in the thermal infrared". Journal of Geophysical Research 108 (8). 
  31. ^ Mars General Circulation Modeling Group. "Mars' low surface pressure.". NASA. Retrieved February 22, 2007. 
  32. ^ Mars General Circulation Modeling Group. "Mars' desert surface.". NASA. Retrieved February 25, 2007. 
  33. ^ Antares project "Mars Small-Scale Weather" (MSW)
  34. ^ a b François Forget. "Alien Weather at the Poles of Mars". Science. Retrieved February 25, 2007. 
  35. ^ Mars General Circulation Modeling Group. "The Martian tropics...". NASA. Retrieved September 8, 2007. 
  36. ^ NASA. "Planet Gobbling Dust Storms". NASA. Retrieved February 22, 2007. 
  37. ^ a b c Fenton, Lori K.; Geissler, Paul E.; Haberle, Robert M. (2007). "Global warming and climate forcing by recent albedo changes on Mars". Nature 446 (7136): 646–649. Bibcode:2007Natur.446..646F. doi:10.1038/nature05718. PMID 17410170. 
  38. ^ Mars Exploration Rover Status Report Concern Increasing About Opportunity
  39. ^ "Duststorms on Mars". whfreeman.com. Retrieved February 22, 2007. 
  40. ^ Zurek, Richard W.; Martin, Leonard J. (1993). "Interannual variability of planet-encircling dust storms on Mars". Journal of Geophysical Research (Journal of Geophysical Research) 98 (E2): 3247–3259. Bibcode:1993JGR....98.3247Z. doi:10.1029/92JE02936. Retrieved March 16, 2007. 
  41. ^ G. Landis, et al., "Dust and Sand Deposition on the MER Solar Arrays as Viewed by the Microscopic Imager," 37th Lunar and Planetary Science Conference, Houston TX, March 13–17, 2006. pdf file (also summarized in NASA Glenn Research and Technology 2006 report)
  42. ^ Kok, Jasper F.; Renno, Nilton O. (2008). "Electrostatics in Wind-Blown Sand". Physical Review Letters 100 (1): 014501. arXiv:0711.1341. Bibcode:2008PhRvL.100a4501K. doi:10.1103/PhysRevLett.100.014501. PMID 18232774. 
  43. ^ Almeida, Murilo P. et al. (2008). "Giant saltation on Mars". PNAS 105 (17): 6222–6226. Bibcode:2008PNAS..105.6222A. doi:10.1073/pnas.0800202105. PMC 2359785. PMID 18443302. 
  44. ^ a b c d Mars Global Surveyor - "8 Year Anniversary"
  45. ^ a b c d e f David Brand and Ray Villard (May 19, 1999). "Colossal cyclone swirling near Martian north pole is observed by Cornell-led team on Hubble telescope". Cornell News. Retrieved September 6, 2007. 
  46. ^ Mumma, M. J.; Novak, R. E.; DiSanti, M. A.; Bonev, B. P., "A Sensitive Search for Methane on Mars" (abstract only). American Astronomical Society, DPS meeting #35, #14.18.
  47. ^ Michael J. Mumma. "Mars Methane Boosts Chances for Life". Skytonight.com. Archived from the original on February 20, 2007. Retrieved February 23, 2007. 
  48. ^ V. Formisano, S. Atreya T. Encrenaz, N. Ignatiev, M. Giuranna (2004). "Detection of Methane in the Atmosphere of Mars". Science 306 (5702): 1758–1761. Bibcode:2004Sci...306.1758F. doi:10.1126/science.1101732. PMID 15514118. 
  49. ^ Francis Reddy (March 7, 2006). "Titan, Mars methane may be on ice". Astronomy Magazine. Retrieved September 6, 2007. 
  50. ^ V. Formisano, S. Atreya, T. Encrenaz, N. Ignatiev, M. Giuranna (2004). "Detection of Methane in the Atmosphere of Mars". Science 306 (5702): 1758–1761. Bibcode:2004Sci...306.1758F. doi:10.1126/science.1101732. PMID 15514118. 
  51. ^ a b "Mars Express confirms methane in the Martian atmosphere". ESA. March 30, 2004. Retrieved August 19, 2008. 
  52. ^ V. A. Krasnopolskya, J. P. Maillard, T. C. Owen (2004). "Detection of methane in the Martian atmosphere: evidence for life?". Icarus 172 (2): 537–547. Bibcode:2004Icar..172..537K. doi:10.1016/j.icarus.2004.07.004. 
  53. ^ Zahnle, Kevin; Freedman, Richard S.; Catling, David C., [1] (abstract only). Icarus, Volume 212, Issue 2, p. 493-503.
  54. ^ Martin Baucom (2006). "Life on Mars?". American Scientist 94 (2). Archived from the original on February 23, 2006. Retrieved February 26, 2007. 
  55. ^ Thomas, Caroline; et al. (January 2009). "Variability of the methane trapping in Martian subsurface clathrate hydrates". Planetary and Space Science 57 (1): 42–47. arXiv:0810.4359. Bibcode:2009P&SS...57...42T. doi:10.1016/j.pss.2008.10.003. Retrieved August 2, 2009. 
  56. ^ Tazaz, Amanda M.; Bebout, Brad M.; Kelley, Cheryl A.; Poole, Jennifer; Chanton, Jeffrey P. [2] (abstract only). Icarus, Volume 224, Issue 2, p. 268-275.
  57. ^ Tenenbaum, David (June 9, 2008). "Making Sense of Mars Methane". Astrobiology Magazine. Archived from the original on September 23, 2008. Retrieved October 8, 2008. 
  58. ^ "Mars Curiosity Rover News Telecon -November 2, 2012". 
  59. ^ Kerr, Richard A. (November 2, 2012). "Curiosity Finds Methane on Mars, or Not". Science (journal). Retrieved November 3, 2012. 
  60. ^ Wall, Mike (November 2, 2012). "Curiosity Rover Finds No Methane on Mars —Yet". Space.com. Retrieved November 3, 2012. 
  61. ^ Chang, Kenneth (November 2, 2012). "Hope of Methane on Mars Fades". New York Times. Retrieved November 3, 2012. 
  62. ^ Webster, Christopher R.; Mahaffy, Paul R.; Atreya, Sushil K.; Flesch, Gregory J.; Farley, Kenneth A. (September 19, 2013). "Low Upper Limit to Methane Abundance on Mars". Science. doi:10.1126/science.1242902. Retrieved September 19, 2013. 
  63. ^ Staff (September 2012). "Mangalyaan -Mission Objectives". Indian Space Science Data Centre. Retrieved October 8, 2013. 
  64. ^ Rincon, Paul (July 9, 2009). "Agencies outline Mars initiative". BBC News. Retrieved July 26, 2009. 
  65. ^ "NASA orbiter to hunt for source of Martian methane in 2016". Thaindian News. March 6, 2009. Retrieved July 26, 2009. 
  66. ^ a b Chang, Kenneth (December 12, 2007). "Mars Rover Finding Suggests Once Habitable Environment". The New York Times. Retrieved April 30, 2010. 
  67. ^ Mars General Circulation Modeling Group. "The Martian mountain ranges...". NASA. Retrieved September 8, 2007. 
  68. ^ "PIA04294: Repeated Clouds over Arsia Mons". NASA. Retrieved September 8, 2007. 
  69. ^ a b Benson et al. (2006). "Interannual variability of water ice clouds over major martian volcanoes observed by MOC". Icarus 184 (2): 365–371. Bibcode:2006Icar..184..365B. doi:10.1016/j.icarus.2006.03.014. 
  70. ^ Darling, David. "Mars, polar caps, ENCYCLOPEDIA OF ASTROBIOLOGY, ASTRONOMY, AND SPACEFLIGHT". Retrieved February 26, 2007. 
  71. ^ Mars General Circulation Modeling Group. "Mars' dry ice polar caps...". NASA. Retrieved February 22, 2007. 
  72. ^ "MIRA's Field Trips to the Stars Internet Education Program". Mira.org. Retrieved February 26, 2007. 
  73. ^ Carr, Michael H. (2003). "Oceans on Mars: An assessment of the observational evidence and possible fate". Journal of Geophysical Research 108 (5042): 24. Bibcode:2003JGRE..108.5042C. doi:10.1029/2002JE001963. 
  74. ^ Phillips, Tony. "Mars is Melting, Science at NASA". Retrieved February 26, 2007. 
  75. ^ Pelletier, J. D. (2004). "How do spiral troughs form on Mars?". Geology 32 (4): 365–367. Bibcode:2004Geo....32..365P. doi:10.1130/G20228.2. Retrieved February 27, 2007. 
  76. ^ "Mars Polar Cap Mystery Solved". Mars Today. March 25, 2004. Retrieved January 23, 2007. 
  77. ^ Smith, Isaac B.; Holt, J. W. (2010). "Onset and migration of spiral troughs on Mars revealed by orbital radar". Nature 465 (4): 450–453. Bibcode:2010Nature....32..450P. doi:10.1038/nature09049. 
  78. ^ "Mystery Spirals on Mars Finally Explained". Space.com. May 26, 2010. Retrieved May 26, 2010. 
  79. ^ Burnham, Robert (August 16, 2006). "Gas jet plumes unveil mystery of 'spiders' on Mars". Arizona State University web site. Retrieved August 29, 2009. 
  80. ^ Kieffer, Hugh H.; Christensen, Philip R.; Titus, Timothy N. (August 17, 2006). "CO2 jets formed by sublimation beneath translucent slab ice in Mars' seasonal south polar ice cap". Nature (Nature Publishing Group) 442 (7104): 793–796. Bibcode:2006Natur.442..793K. doi:10.1038/nature04945. PMID 16915284. Retrieved August 31, 2009. 
  81. ^ The Solar Wind at Mars
  82. ^ Madeleine, J. et al. 2007. Mars: A proposed climatic scenario for northern mid-latitude glaciation. Lunar Planet. Sci. 38. Abstract 1778.
  83. ^ Madeleine, J. et al. 2009. Amazonian northern mid-latitude glaciation on Mars: A proposed climate scenario. Icarus: 203. 300-405.
  84. ^ Mischna, M. et al. 2003. On the orbital forcing of martian water and CO2 cycles: A general circulation model study with simplified volatile schemes. J. Geophys. Res. 108. (E6). 5062.
  85. ^ Touma J. and J. Wisdom. 1993. The Chaotic Obliquity of Mars" Science 259, 1294–1297.
  86. ^ Laskar, J., A. Correia, M. Gastineau, F. Joutel, B. Levrard, and P. Robutel. 2004. Long term evolution and chaotic diffusion of the insolation quantities of Mars" Icarus 170, 343-364.
  87. ^ Levy, J., J. Head, D. Marchant, D. Kowalewski. 2008. Identification of sublimation-type thermal contraction crack polygons at the proposed NASA Phoenix landing site: Implications for substrate properties and climate-driven morphological evolution. Geophys. Res. Lett. 35. doi:10.1029/2007GL032813
  88. ^ Levy, J., J. Head, D. Marchant. 2009a. Thermal contraction crack polygons on Mars: Classification, distribution, and climate implications from HiRISE observations. J. Geophys. Res. 114. doi:10.1029/2008JE003273
  89. ^ Hauber, E., D. Reiss, M. Ulrich, F. Preusker, F. Trauthan, M. Zanetti, H. Hiesinger, R. Jaumann, L. Johansson, A. Johnsson, S. Van Gaselt, M. Olvmo. 2011. Landscape evolution in Martian mid-latitude regions: insights from analogous periglacial landforms in Svalbard. In: Balme, M., A. Bargery, C. Gallagher, S. Guta (eds). Martian Geomorphology. Geological Society, London. Special Publications: 356. 111-131
  90. ^ Laskar, J., A. Correia, M. Gastineau, F. Joutel, B. Levrard, and P. Robutel. 2004. Long term evolution and chaotic diffusion of the insolation quantities of Mars" Icarus 170, 343-364.
  91. ^ a b Mellon, M., B. Jakosky. 1995. The distribution and behavior of Martian ground ice during past and present epochs" J. Geophys. Res. 100, 11781–11799.
  92. ^ Schorghofer, N., 2007. Dynamics of ice ages on Mars" Nature 449, 192–194.
  93. ^ Madeleine, J., F. Forget, J. Head, B. Levrard, F. Montmessin. 2007. Exploring the northern mid-latitude glaciation with a general circulation model. In: Seventh International Conference on Mars. Abstract 3096.
  94. ^ a b Steinn Sigurðsson. "Global warming on Mars?". RealClimate. Retrieved February 21, 2007. 
  95. ^ Jacques Laskar (September 25, 2002). "Martian 'wobbles' shift climate". BBC. Retrieved February 24, 2007. 
  96. ^ Francis Reddy. "Titan, Mars methane may be on ice". Astronomy Magazine. Retrieved March 16, 2007. 
  97. ^ a b Malin, M. et al. 2010. An overview of the 1985–2006 Mars Orbiter Camera science investigation. MARS INFORMATICS. http://marsjournal.org
  98. ^ "MOC Observes Changes in the South Polar Cap". Malin Space Science Systems. Retrieved February 22, 2007. 
  99. ^ "Evaporating ice". Astronomy.com. Retrieved February 22, 2007. 
  100. ^ Orbiter's Long Life Helps Scientists Track Changes on Mars
  101. ^ Mars Emerging from Ice Age, Data Suggest
  102. ^ Colaprete, A; Barnes, JR; Haberle, RM; Hollingsworth, JL; Kieffer, HH; Titus, TN (May 12, 2005). "Albedo of the South Pole of Mars.". Nature 435 (7039): 184–188. Bibcode:2005Natur.435..184C. doi:10.1038/nature03561. PMID 15889086. 
  103. ^ Jakosky, Bruce M.; Haberle, Robert M. (1990). "Year-to-year instability of the Mars Polar Cap". J.Geophys Res 95: 1359–1365. Bibcode:1990JGR....95.1359J. doi:10.1029/JB095iB02p01359. 
  104. ^ Access : Hot times in the Solar System : Nature News
  105. ^ "Look to Mars for the truth on global warming". National Post. Retrieved March 2, 2007. 
  106. ^ "Global warming on Mars, ice caps melting". Skeptical Science. Retrieved September 17, 2013. 
  107. ^ Ker Than (March 12, 2007). "Sun Blamed for Warming of Earth and Other Worlds". Live Science. Retrieved September 6, 2007. 
  108. ^ Kate Ravilious. "Mars Melt Hints at Solar, Not Human, Cause for Warming, Scientist Says". National Geographic Society. Retrieved March 2, 2007. 
  109. ^ Hargitai Henrik (2009). "Climate Zones of Mars". Lunar and Planetary Institute. Retrieved May 18, 2010. 
  110. ^ "Curiosity rover touches down on Mars". CBS News. 

Further reading[edit]

  • Jakosky, Bruce M.; Phillips, Roger J. (2001). "Mars' volatile and climate history". Nature 412 (6843): 237–244. doi:10.1038/35084184.  review article

External links[edit]