The Mercury

Currently available knowledge about the planet Mercury has been obtained, mainly, using the spacecraft Mariner-10 and radar observations from the Earth, when in the direction of the planet Mercury impulses of radio waves are transmitted, and then they study their reflection. The planet Mercury is dotted with impact craters. There are long mountain ranges on Mercury that cross crater craters and other geological structures. It should be noted that Mercury does not have its own satellite (at least, it is not found).

The Mercury has heavily cratered uplands (or continents). The lowlands of Mercury are flat plains

The Mercury has heavily cratered uplands (or continents). The lowlands of Mercury are flat plains.

The most important trail of collisions of Mercury with other celestial bodies is the Kaloris basin. The width of this basin is about 1340 km, which makes it one of the largest in the solar system.

The Mercury has a density of 5,4 times the density of water. The reason for such a high density is that Mercury consists mainly of a huge iron core that makes up a large part of the planet. The thickness of the outer layer with respect to the core, the mantle, is no more than 610 km. The presence of the global magnetic field of Mercury, according to many experts, suggests that the outer part of the nucleus is still in a molten state. At the same time, simple calculations show that by now the core should have cooled sufficiently to harden.

The Mercury is surrounded by weak traces of the atmosphere, but they are too insignificant. Due to the lack of atmosphere on the surface of the planet Mercury, very sharp temperature changes from -183 degrees Celsius at night to +440 degrees during the day are observed. Near the northern and southern poles of the planet Mercury, with the help of a radar, regions with a high reflection coefficient were found. This can mean the presence on the poles of large ice caps located in deep craters, the bottom of which is never illuminated by the Sun.

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