Can the atmospheric pressure on the surface of Mars increase to the size of the Earth s surface?

It is possible to inject enough other gases into the Martian atmosphere using artificial methods, but the engineering is very huge, and the possibility is very small, but it is achievable in principle.

Mars is also surrounded by an atmosphere, similar to Earth's. The main component of the Martian atmosphere is carbon dioxide, followed by nitrogen and argon, in addition to small amounts of oxygen and water vapor. The presence of nitrogen in both the Martian atmosphere and the Earth's atmosphere is the biggest similarity between Mars and Earth.

The Martian atmosphere is less than one percent of the Earth's atmosphere, with a surface atmospheric pressure of 500,700 Pa. The vertical distribution of the temperature of the Martian atmosphere is different from that of Earth: from the surface to an altitude of 50 km.

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As far as is known, the Martian atmosphere is dominated by carbon dioxide, which is very thin and cold.

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Mars' atmosphere is only about 1% of Earth's density, very dry, with a low temperature, an average surface temperature of minus 55, and water and carbon dioxide that freeze easily. In the early days of Mars, it was very similar to Earth. Like Earth, almost all of the carbon dioxide on Mars is converted into carbon-containing rocks.

But without the movement of Earth's tectonic plates, Mars is unable to recycle carbon dioxide into its atmosphere to produce a significant greenhouse effect. Therefore, even if it is pulled to the same distance from the Earth from the Sun, the temperature on the surface of Mars is still much colder than on Earth.

That thin layer of Mars' atmosphere is mostly made up of the remaining carbon dioxide (plus nitrogen (argon) and trace amounts of oxygen (and water vapor). The pure mean atmospheric pressure on the surface of Mars is only about 7 millibars (less than 1% of Earth's), but it varies with altitude, reaching as high as 9 millibars at the deepest part of the basin and only 1 millibar at the top of the Olympian Mountains. But it's also strong enough to support the occasional hurricane and storm that sweeps across the planet throughout the month.

The thin layers of Mars' atmosphere can also contribute to the greenhouse effect, but they only raise the temperature of its surface5 much less than what we know about Venus and Earth.

The poles of Mars are permanently covered with solid carbon dioxide (dry ice). The structure of this ice cover is cascading, which is made up of layers of ice and changing layers of carbon dioxide in turn. In the northern summer, carbon dioxide is completely sublimated, leaving behind a layer of icy water.

Since carbon dioxide has never completely disappeared in the south, there is no way to know whether there is also an ice-water layer under the ice in the south (left).The cause of this phenomenon is unknown, but it may be due to a change in climate caused by long-term changes in the angle between the equatorial plane of Mars and its orbit. Perhaps there is also water deeper below the surface of Mars.

This change in the polar cover due to seasonal changes has changed the pressure of Mars by about 25%. (measured by the Corsair).However, recent observations through the Hubble telescope have shown that the environment at the time of the Corsair's survey was not typical.

Mars' atmosphere now appears to be colder and drier than the Viking surveyed.

Venus and Mars have weather as we know it. Because the axis of Venus is hardly tilted, it lacks seasonal changes: it is hot at all times.

The atmosphere is 95% carbon dioxide, which heats the surface of Venus through the greenhouse effect, reaching an average temperature of 885°F (457).

Venus's surface pressure is 90 standard atmospheres (91,192 millibars), while the Earth's surface pressure is 1 standard atmosphere (1013 millibars), and a violent easterly wind orbits Venus at 200 miles (322 kilometers) per hour, making it windy. Light pours out through thick clouds of sulfuric acid, making Venus sparkle in the night sky.

The Martian atmosphere contains 95% carbon dioxide, but it has a relatively small gravitational pull. Most of its original gas has been blown away by the solar wind. The average surface pressure on Mars is standard atmospheric pressure (8 mbar).

Low air pressure, combined with extreme dryness, prevents water from accumulating. This means that Mars has almost no clouds, and its thin atmosphere makes it quite sensitive to the Sun's heat: for example, the temperature at the equator fluctuates from -193°F to +72°F (-125 to +22) throughout the year.

The ice covers the poles of Mars, and their melting and freezing are affected by the distance between Mars and the Sun, as well as by winds traveling at 125 miles (200 kilometers) per hour, which create powerful dust clouds that block the sun's rays and slow down the melting of the ice. These dust storms often plague entire stars.

It turns out that since Mars does not have a global magnetic field, the solar wind can directly reach Mars and drive away charged ions in the upper atmosphere of Mars. And the earth we are in, due to the protection of the magnetic field, the charged solar wind ions cannot directly reach the earth's atmosphere. As a result, solar wind ions have different effects on the atmosphere on Earth and Mars.

Scientists believe that the water on Mars exists below the surface of Mars by sedimentary rocks.