Like any large planet, Mars has an atmosphere. It consists of a gaseous substance that the planet holds due to gravity. However, the air on Mars is very different from the earth.
General information about the atmosphere of Mars
The atmosphere of Mars is much thinner than that of Earth. Its height is 11 km, which is approximately 9-10% of the earth. It's caused weak force gravity on a planet unable to hold onto a wider layer of gas. The small thickness and density of the atmosphere causes such air phenomena that cannot be found on Earth.
Chemically, the atmosphere consists mainly of carbon dioxide.
The density of the atmosphere is also very low: more than 61 times less than the average density on Earth.
Due to its properties, the atmosphere is constantly exposed to the solar wind, losing matter and dispersing faster than on other planets. This process is called dissipation. This is because the planet Mars does not have a magnetic field.
Atmospheric structure
Even being thin, the Martian atmosphere is heterogeneous and has a layered structure. Its structure looks like this:
● Below all layers is the troposphere. It occupies the entire space from the surface to 20-30 km. The temperature here decreases evenly as it rises. The upper limit of the troposphere is not fixed, and changes its position throughout the year.
● Above is the stratomesosphere. The temperature in this part is approximately the same and equal to -133 ° C. It continues up to a height of 100 km above the surface, where the entire lower atmosphere ends with it.
● Everything above (up to the border where space begins) is called the upper atmosphere. Another name for this layer is the thermosphere, and its average temperature is from 200 to 350 K.
● Inside it stands out the ionosphere, which, as the name implies, is characterized by high level ionization due to solar radiation. It begins approximately in the same place as the entire upper part and has a length of approximately 400 km.
● At an altitude of about 230 km, the thermosphere ends. Its last layer is called ecobase.
● Not belonging to either the lower or upper atmosphere determine the chemosphere in which chemical reactions initiated by light. Due to the absence of any analogue of the Earth's Ozone layer on Mars, this layer begins at the surface level. And it ends at an altitude of 120 km.
So, the surface of Mars is covered with a rather thin and rarefied atmosphere, which, however, has a relatively complex structure. In total, the atmosphere of Mars consists of seven layers, but this number may vary in different sources, since scientists have not yet agreed on the nature of some layers.
Do not think that the layered structure indicates static. The atmosphere of Mars is also prone to change, like the earth's: it has both general circulation and partial movements of air currents.
Composition of the atmosphere
The chemical composition of the atmosphere of Mars is very different from that of Earth. The air on Mars is made up of the following gases:
● The basis of the atmosphere of the planet Mars is carbon dioxide. It occupies about 95% of its volume. It's the only one heavy gas that the planet can hold.
● The majority of carbon dioxide is CO2, but carbon monoxide CO also makes up a portion of it. This proportion is unusually small and leads scientists to theorize why CO is not accumulating.
● Nitrogen N2. It makes up a very small part of the atmosphere - only 2.7%. However, it can linger in the atmosphere only in the form of a double molecule. Radiation from the Sun constantly splits atmospheric nitrogen into atoms, after which it dissipates.
● Argon occupies 1.6% and is represented mainly by the heavy isotope argon-40.
● There is also oxygen on Mars, but it is contained mainly in the upper atmosphere and appears during the decomposition of other substances, from where it then passes to the lower layers. Because of this, at an altitude of about 110 km and above, there is 3-4 times more O2 than below this level. They cannot breathe.
● Ozone is the most uncertain gas in the Martian atmosphere. Its content depends on the air temperature, and therefore on the time of year, latitude and hemisphere.
● Methane on Mars, despite its low content in the atmosphere, is one of the most mysterious gases on the planet. It can have several sources, but two of the most relevant are: the influence of temperatures (for example, in volcanoes) and the processing of substances by bacteria and ruminants, after which bacterial methane is formed. The latter is of particular interest to astrobiology - it is what they are looking for on potentially inhabited planets to prove that they have life. What methane that appears on Mars in bursts can indicate is unknown.
● organic compounds, such as H2CO, HCl, and SO2, are also found in the Martian atmosphere. They can clarify the issue discussed above, since their presence indicates the absence of volcanic activity - and therefore thermogenic methane.
● Water. Although its content is several hundred times less than in the driest regions of the Earth, it is still present.
● It is also worth mentioning that the atmosphere of Mars is filled with the smallest dust particles (mainly iron oxide). They make the atmosphere reddish-orange from the outside, and they are also responsible for the colors of the sky, the opposite of Earth: the daytime skies on Mars are yellow-brown, at sunset and dawn they turn pink, and around the Sun they are blue.
Clouds
The atmosphere of the Red Planet is capable of forming the same phenomena as the earth's. For example, there are clouds on Mars.
Vaporous water in the atmosphere of the planet Mars is extremely small, but still enough for the formation of clouds. Most often they are located at a height of one to three tens of kilometers above the surface. Concentrated water vapor collects into clouds mainly at the equator - where they can be observed all year round.
In addition, the cloud on Mars can also form CO2. Usually it is located above water (at an altitude of about 20 km).
There are also fogs on Mars. Most often - in lowlands and craters, at night.
Once upon a time, vortex-like systems of clouds were discovered in a picture of the Martian atmosphere. This was evidence of a more complex climatic phenomenon - a cyclone. On Earth, this is a common occurrence, but on other planets it is quite unusual. Nothing more is known about Martian cyclones yet.
There is no ordinary rain on Mars, but among natural phenomena sometimes there is a virga - drops or snow that evaporate in the air, not reaching the ground.
Greenhouse effect
The greenhouse effect on Mars is always discussed in the context of the discussion of liquid water that once existed on it. “Rivers” on the surface are already talking about this, but this was not enough for scientists, and they decided to find what allowed liquid H2O to appear.
When Mars was a young planet, its volcanoes were extremely active. Each volcanic explosion on Mars released carbon dioxide and methane, which decomposed under the action of sunlight, producing hydrogen and creating a “hydrogen greenhouse effect”. At some point, the concentration of the latter gas increased so much that it allowed the existence of lakes, rivers and even entire oceans of water. However, over time, the planet's atmosphere became thinner and could no longer provide conditions in which water would remain liquid. Right now, only water vapor or ice can be found on Mars. Transition from one state of aggregation to another it occurs by means of sublimation, bypassing the liquid stage. This can be called a unique feature in the history of the atmosphere of Mars, since this has not yet happened on any other planet. However, this is only a scientific theory.
Pressure
Average Atmosphere pressure on Mars is 4.5 mmHg or 600 Pascals. This is one 169th of the average pressure on Earth. Such pressure makes it impossible for a person to survive on the surface without a spacesuit. People stranded on the open surface of the planet Mars without protection face instant death. The reason for this is the existence of the so-called Armstrong limit - the pressure level at which water boils at normal human body temperature. The pressure of the atmosphere on the surface of Mars is well below this limit.
dust devils
Dust storms that regularly occur on Mars are a feature of this planet. Their cause is storms on Mars, in which wind speeds reach 100 km / h. Air collects dust hanging in the atmosphere to a height of up to 50 km. This generates on Mars the very dust storms. Most often they occur in the polar regions and rage for 1.5 - 3 months. Similarly, sandstorms occur on Mars. The only difference is that this time larger particles rise into the air, which have settled on the surface - sand.
However, if there is wind on Mars, then there must be dangerous air phenomena that it causes. For example, tornadoes. They, like storms, raise sand and dust into the air, but extend hundreds of meters wide and kilometers high and seem much more dangerous (even though their speed is three times lower than that of storms - only 30 km /h). Due to the same low density of the atmosphere, tornadoes on Mars look more like tornadoes. Their second name is dust devils. From orbit you can see how they leave black swirling tracks on a light sandy surface.
Radiation
Radiation on Mars is no less dangerous for people than dust or low pressure. There are two reasons for this: the weakness and rarefaction of the atmosphere and the absence of a magnetosphere near the planet Mars. The air part is not able to protect its surface from cosmic radiation. That is why in a few days spent on the planet without protection, the astronaut will receive an annual dose of radiation.
Terraforming
Despite all this, people still dream of subjugating Mars and even making it habitable. The atmosphere of Mars is one of the main obstacles on this path. However, the terraforming of Mars is proposed to be carried out not only by providing it with oxygen and dense atmosphere, but also creating a major source of space fuel. It is proposed to chemically decompose carbon dioxide into oxygen and CO, which can be used to provide a colony and fuel transport in order to establish a connection with the Earth.
Characteristics: The atmosphere of Mars is thinner than the atmosphere of the Earth. In composition, it resembles the atmosphere of Venus and consists of 95% carbon dioxide. About 4% is accounted for by nitrogen and argon. Oxygen and water vapor in the Martian atmosphere is less than 1% (See exact composition). The average pressure of the atmosphere at the surface level is about 6.1 mbar. This is 15,000 times less than on Venus, and 160 times less than at the surface of the Earth. In the deepest depressions, the pressure reaches 10 mbar.
The average temperature on Mars is much lower than on Earth - about -40 ° C. Under the most favorable conditions in the summer in the daytime half of the planet, the air warms up to 20 ° C - quite an acceptable temperature for the inhabitants of the Earth. But on a winter night, frost can reach up to -125 ° C. At winter temperatures, even carbon dioxide freezes, turning into dry ice. Such sharp temperature drops are caused by the fact that the rarefied atmosphere of Mars is not able to retain heat for a long time. The first measurements of the temperature of Mars using a thermometer placed at the focus of a reflecting telescope were carried out as early as the early 1920s. Measurements by W. Lampland in 1922 gave an average surface temperature of Mars of -28°C, E. Pettit and S. Nicholson in 1924 obtained -13°C. A lower value was obtained in 1960. W. Sinton and J. Strong: -43°C. Later, in the 50s and 60s. Numerous temperature measurements were accumulated and summarized at various points on the surface of Mars, in different seasons and times of the day. From these measurements, it followed that during the day at the equator the temperature can reach up to +27°C, but by morning it can reach -50°C.
There are also temperature oases on Mars, in the areas of the "lake" Phoenix (Sun Plateau) and the land of Noah, the temperature difference is from -53 ° C to + 22 ° C in summer and from -103 ° C to -43 ° C in winter. So, Mars is a very cold world, but the climate there is not much harsher than in Antarctica. When the first photographs of the surface of Mars taken by the Viking were transmitted to Earth, scientists were very surprised to see that the Martian sky was not black, as expected, but pink. It turned out that the dust hanging in the air absorbs 40% of the incoming sunlight, creating a color effect.
Dust storms: Winds are one of the manifestations of temperature difference. Strong winds often blow over the surface of the planet, the speed of which reaches 100 m/s. Low gravity allows even rarefied air currents to raise huge clouds of dust. Sometimes quite vast areas on Mars are covered by grandiose dust storms. Most often they occur near the polar caps. A global dust storm on Mars prevented photographing the surface from the Mariner 9 probe. It raged from September 1971 to January 1972, raising about a billion tons of dust into the atmosphere at an altitude of more than 10 km. Dust storms most often occur during periods of great opposition, when summer in the southern hemisphere coincides with the passage of Mars through perihelion. Duration of storms can reach 50-100 days. (Previously, the changing color of the surface was explained by the growth of Martian plants).
Dust Devils: dust devils is another example of temperature-related processes on Mars. Such tornadoes are very frequent manifestations on Mars. They raise dust into the atmosphere and arise due to temperature differences. Reason: during the day, the surface of Mars heats up enough (sometimes to positive temperatures), but at a height of up to 2 meters from the surface, the atmosphere remains just as cold. Such a drop causes instability, raising dust into the air - dust devils are formed.
Water vapor: There is very little water vapor in the Martian atmosphere, but at low pressure and temperature, it is in a state close to saturation, and often collects in clouds. Martian clouds are rather inexpressive compared to those on Earth. Only the largest of them are visible through a telescope, but observations from spacecraft have shown that on Mars there are clouds of a wide variety of shapes and types: cirrus, wavy, leeward (near large mountains and under the slopes of large craters, in places protected from the wind). Over the lowlands - canyons, valleys - and at the bottom of the craters in the cold time of the day there are often fogs. In the winter of 1979, a thin layer of snow fell in the Viking-2 landing area, which lay for several months.
Seasons: At the moment it is known that of all the planets of the solar system, Mars is the most similar to the Earth. It formed approximately 4.5 billion years ago. The axis of rotation of Mars is inclined to its orbital plane by approximately 23.9 °, which is comparable to the tilt of the Earth's axis, which is 23.4 °, and therefore there, as on Earth, there is a change of seasons. Seasonal changes are most pronounced in the polar regions. IN winter time polar caps occupy a significant area. The boundary of the northern polar cap can move away from the pole by a third of the distance to the equator, and the boundary of the southern cap overcomes half this distance. This difference is due to the fact that in the northern hemisphere winter occurs when Mars passes through the perihelion of its orbit, and in the southern hemisphere when it passes through aphelion. Because of this, winters in the southern hemisphere are colder than in the northern. And the duration of each of the four Martian seasons varies depending on its distance from the Sun. Therefore, in the Martian northern hemisphere, winters are short and relatively "moderate", and summers are long, but cool. In the south, on the contrary, summers are short and relatively warm, and winters are long and cold.
With the onset of spring, the polar cap begins to "shrink", leaving behind gradually disappearing islands of ice. At the same time, a so-called wave of darkening propagates from the poles to the equator. Modern theories explain it by the fact that spring winds carry large masses of soil along the meridians with different reflective properties.
Apparently, none of the caps disappear completely. Before the start of exploration of Mars with the help of interplanetary probes, it was assumed that its polar regions were covered with frozen water. More accurate modern ground and space measurements have also found frozen carbon dioxide in the composition of Martian ice. In summer, it evaporates and enters the atmosphere. The winds carry it to the opposite polar cap, where it freezes again. This cycle of carbon dioxide and the different sizes of the polar caps explain the variability in the pressure of the Martian atmosphere.
A Martian day, called a sol, is 24.6 hours long and its year is sol 669.
Climate influence: The first attempts to find direct evidence in the Martian soil of the presence of the basis for life - liquid water and elements such as nitrogen and sulfur, were not successful. An exobiological experiment conducted on Mars in 1976 after landing on its surface by the American Viking interplanetary station carrying an automatic biological laboratory (ABL) on its board did not provide evidence for the existence of life. Absence organic molecules on the studied surface could be caused by the intense ultraviolet radiation of the Sun, since Mars does not have a protective ozone layer, and the oxidizing composition of the soil. Therefore, the upper layer of the Martian surface (about a few centimeters thick) is barren, although there is an assumption that conditions that were billions of years ago have been preserved in deeper, subsurface layers. A certain confirmation of these assumptions was recently discovered on Earth at a depth of 200 m microorganisms - methanogens that feed on hydrogen and breathe carbon dioxide. A specially conducted experiment by scientists proved that such microorganisms could survive in the harsh Martian conditions. The hypothesis of a warmer ancient Mars with open water bodies - rivers, lakes, and maybe seas, as well as with a denser atmosphere - has been discussed for more than two decades, since it would be very difficult. In order to exist on Mars liquid water, its atmosphere would have to be very different from the current one.
Variable Martian climate Modern Mars is a very inhospitable world. The rarefied atmosphere, which is also unsuitable for breathing, terrible dust storms, lack of water and sudden temperature changes during the day and year - all this indicates that it will not be so easy to populate Mars. But once upon a time, rivers flowed on it. Does this mean that Mars had a different climate in the past? |
Acquaintance with any planet begins with its atmosphere. It envelops the cosmic body and protects it from external influences. If the atmosphere is very rarefied, then such protection is extremely weak, but if it is dense, then the planet is in it like in a cocoon - the Earth can serve as an example here. However, such an example in solar system single and does not extend to other terrestrial planets.
And therefore the atmosphere of Mars (the red planet) is extremely rarefied. Its approximate thickness does not exceed 110 km, and its density in comparison with the Earth's atmosphere is only 1%. In addition to this, the red planet has an extremely weak and unstable magnetic field. As a result, the solar wind invades Mars and disperses atmospheric gases. As a result, the planet loses from 200 to 300 tons of gases per day. It all depends on solar activity and on the distance to the star.
From this it is not difficult to understand why atmospheric pressure is very low. At sea level, it is 160 times smaller than the earth.. On volcanic peaks, it is 1 mm Hg. Art. And in deep depressions, its value reaches 6 mm Hg. Art. The average value on the surface is 4.6 mm Hg. Art. The same pressure is recorded in the Earth's atmosphere at an altitude of 30 km from the Earth's surface. With such values, water cannot be present in a liquid state on the red planet.
The atmosphere of Mars contains 95% carbon dioxide.. That is, we can say that he occupies a dominant position. Nitrogen is in second place. It accounts for almost 2.7%. The third place is occupied by argon - 1.6%. And oxygen is in fourth place - 0.16%. There are also small amounts of carbon monoxide, water vapor, neon, krypton, xenon, and ozone.
The composition of the atmosphere is such that it is impossible for people to breathe on Mars. You can only move around the planet in a spacesuit. At the same time, it should be noted that all gases are chemically inert and there is not a single poisonous one among them. If the pressure on the surface were at least 260 mm Hg. Art., then it would be possible to move along it without a spacesuit in ordinary clothes, having only a breathing apparatus.
Some experts believe that a few billion years ago, the atmosphere of Mars was much denser and richer in oxygen. On the surface there were rivers and lakes of water. This is indicated by numerous natural formations resembling dried up riverbeds. Their age is estimated at about 4 billion years.
Due to the high rarefaction of the atmosphere, the temperature on the red planet is characterized by high instability. There are sharp diurnal fluctuations, as well as a high temperature difference depending on the latitudes. The average temperature is -53 degrees Celsius. In summer, at the equator, the average temperature is 0 degrees Celsius. At the same time, it can fluctuate in the daytime from +30 to -60 at night. But at the poles there are temperature records. There the temperature can drop to -150 degrees Celsius.
Despite the low density, winds, tornadoes, and storms are often observed in the atmosphere of Mars. The wind speed reaches 400 km/h. It lifts up the pink Martian dust, and it closes the surface of the planet from the prying eyes of people.
I must say that although the Martian atmosphere is weak, it has enough strength to withstand meteorites. Uninvited guests from space, falling to the surface, partially burn out, and therefore there are not so many craters on Mars. Small meteorites burn up in the atmosphere completely and do not cause any harm to the Earth's neighbor.
Vladislav Ivanov
| Carbon dioxide | 95,32 % |
| Nitrogen | 2,7 % |
| Argon | 1,6 % |
| Oxygen | 0,13 % |
| Carbon monoxide | 0,07 % |
| water vapor | 0,03 % |
| Nitric oxide(II) | 0,013 % |
| Neon | 0,00025 % |
| Krypton | 0,00003 % |
| Xenon | 0,000008 % |
| Ozone | 0,000003 % |
| Formaldehyde | 0,0000013 % |
Atmosphere of Mars- the gaseous envelope surrounding the planet Mars. Significantly different from the earth's atmosphere chemical composition, as well as physical parameters. The pressure at the surface is 0.7-1.155 kPa (1/110 of the earth's, or equal to the earth's at an altitude of more than thirty kilometers from the Earth's surface). The approximate thickness of the atmosphere is 110 km. The approximate mass of the atmosphere is 2.5 10 16 kg. Mars has a very weak magnetic field (compared to Earth's), and as a result, the solar wind causes atmospheric gases to dissipate into space at a rate of 300±200 tons per day (depending on current solar activity and distance from the Sun).
Chemical composition
4 billion years ago, the atmosphere of Mars contained an amount of oxygen comparable to its share on the young Earth.
Temperature fluctuations
Since the atmosphere of Mars is very rarefied, it does not smooth out daily fluctuations in surface temperature. Temperatures at the equator range from +30°C during the day to -80°C at night. Temperatures can drop to -143°C at the poles. However, diurnal temperature fluctuations are not as significant as on the atmosphereless Moon and Mercury. Low density does not prevent the atmosphere from forming large-scale dust storms and tornadoes, winds, fogs, clouds, and affecting the climate and the surface of the planet.
The first measurements of the temperature of Mars using a thermometer placed at the focus of a reflecting telescope were made back in the early 1920s. Measurements by W. Lampland in 1922 gave an average surface temperature of Mars of 245 (−28°C), E. Pettit and S. Nicholson in 1924 obtained 260 K (−13°C). A lower value was obtained in 1960 by W. Sinton and J. Strong: 230 K (−43°C).
annual cycle
The mass of the atmosphere during the year varies greatly due to the condensation in the polar caps of large volumes of carbon dioxide in winter and evaporation in summer.
Every planet is different from the rest in a number of ways. People compare other found planets with the one they know well, but not perfectly, - this is the planet Earth. After all, this is logical, life could appear on our planet, which means that if you look for a planet similar to ours, then it will also be possible to find life there. Because of these comparisons, the planets have their own distinctive features. For example, Saturn has beautiful rings, because of which Saturn is called the most beautiful planet in the solar system. Jupiter is the largest planet in the solar system and this feature of Jupiter. So what are the features of Mars? This article is about this.
Mars, like many other planets in the solar system, has moons. Mars has two moons, Phobos and Deimos. The satellites got their names from the Greeks. Phobos and Deimos were the sons of Ares (Mars) and were always close to their father, just as these two satellites are always close to Mars. In translation, “Phobos” means “fear”, and “Deimos” means “horror”.
Phobos is a moon whose orbit is very close to the planet. It is the closest satellite to the planet in the entire solar system. The distance from the surface of Mars to Phobos is 9380 kilometers. The satellite revolves around Mars with a frequency of 7 hours 40 minutes. It turns out that Phobos manages to make three and a few revolutions around Mars, while Mars itself makes one revolution around its axis.
Deimos is the smallest moon in the solar system. The dimensions of the satellite are 15x12.4x10.8 km. And the distance from the satellite to the surface of the planet is 23,450 thousand km. The period of revolution of Deimos around Mars is 30 hours and 20 minutes, which is slightly longer than the time it takes the planet to rotate around its axis. If you are on Mars, then Phobos will rise in the west and set in the east, while making three revolutions per day, and Deimos, on the contrary, will rise in the east and set in the west, while making only one revolution around the planet.
Features of Mars and its Atmosphere
One of the main features of Mars is that it was created. The atmosphere on Mars is very interesting. Now the atmosphere on Mars is very rarefied, it is possible that in the future Mars will completely lose its atmosphere. The features of the atmosphere of Mars are that once upon a time Mars had the same atmosphere and air as on our home planet. But in the course of evolution, the Red Planet lost almost all of its atmosphere. Now the pressure of the atmosphere of the Red Planet is only 1% of the pressure of our planet. Features of the atmosphere of Mars is also that even with three times less gravity of the planet, relative to the Earth, Mars can raise huge dust storms, lifting tons of sand and soil into the air. Dust storms have already spoiled the nerves of our astronomers more than once, since dust storms are very extensive, then observation of Mars from the Earth becomes impossible. Sometimes such storms can even last for months, which greatly spoils the process of studying the planet. But exploration of the planet Mars doesn't stop there. There are robots on the surface of Mars that do not stop the process of exploring the planet.
The atmospheric features of the planet Mars are also in the fact that scientists' guesses about the color of the Martian sky have been refuted. Scientists thought that the sky on Mars should be black, but the pictures taken space station from the planet disproved this theory. The sky on Mars is not black at all, it is pink, thanks to sand and dust particles that are in the air and absorb 40% sunlight, thanks to this, the effect of the pink sky on Mars is created.
Features of the temperature of Mars
Measurements of the temperature of Mars began relatively long ago. It all started with Lampland's measurements in 1922. Then the measurements indicated that the average temperature on Mars is -28º C. Later, in the 50s and 60s, some knowledge about the temperature regime of the planet was accumulated, which were carried out from the 20s to the 60s. From these measurements, it turns out that during the day at the planet's equator the temperature can reach up to +27º C, but by evening it will drop to zero, and by morning it becomes -50º C. The temperature at the poles ranges from +10º C, during the polar day, and to very low temperatures during the polar night.
Features of the relief of Mars
The surface of Mars, like other planets that do not have an atmosphere, is scarred by various craters from falling space objects. Craters are small in size (5 km in diameter) and large (from 50 to 70 km in diameter). Due to the absence of its atmosphere, Mars was subject to meteor showers. But the surface of the planet contains not only craters. Formerly people It was believed that there was never water on Mars, but observations of the surface of the planet tell a different story. The surface of Mars has channels and even small depressions, reminiscent of water deposits. This suggests that there was water on Mars, but for many reasons it disappeared. Now it is difficult to say what needs to be done so that the water on Mars reappears and we could observe the resurrection of the planet.
There are also volcanoes on the Red Planet. The most famous volcano is Mount Olympus. This volcano is known to all those who are interested in Mars. This volcano is the largest hill not only on Mars, but also in the solar system, this is another feature of this planet. If you stand at the foot of Mount Olympus, then it will be impossible to see the edge of this volcano. This volcano is so large that its edges go beyond the horizon and it seems that Olympus is endless.
Features of the magnetic field of Mars
This is probably the last interesting feature this planet. The magnetic field is the protector of the planet, which repels everything electric charges moving towards the planet and repels them from their original trajectory. The magnetic field is completely dependent on the core of the planet. The core on Mars is almost stationary and therefore the planet's magnetic field is very weak. Action magnetic field very interesting, it is not global, as on our planet, but has zones in which it is more active, and in other zones it may not be at all.
Thus, the planet that seems so ordinary to us has a whole set of its own features, some of which are leading in our solar system. Mars is not as simple a planet as you might think at first glance.
