Meteorite hypothesis

There is one interesting hypothesis of the formation of meteorites (the so-called carbonaceous chondrites), which consist of amorphous silicate balls. A number of astronomers are of the opinion about the "hot origin" of such meteorites. However, this requires high temperatures and pressures. Where in the solar system such conditions could develop is not yet clear. Therefore, the question of the origin of carbonaceous chondrites is considered one of the key problems of modern planetary cosmogony.

There is one interesting hypothesis of the formation of meteorites (the so-called carbonaceous chondrites), which consist of amorphous silicate balls

Studying the laws of precipitation of the solid phase from solutions, scientists drew attention to one curious circumstance. It turned out that the process of formation of solid particles in a solution necessarily passes through the stage of formation of amorphous balls, which then gradually crystallize. Further studies showed that the intermediate stage of amorphous balls is characteristic of a very wide class of solutions. Moreover, such balls arise not only in liquid solutions, but also in some cases during the formation of a dust component from the gas phase. Therefore, it can be assumed that the amorphous silicate balls found in chondrites were formed in a "cold" way, during the formation of meteorites from the original cloud from which, according to modern concepts, our entire solar system arose. Then gradually the process of crystallization of the balls, which has not yet been completed.

Since the rate of crystallization of balls depending on temperature is known from laboratory observations, their age can be estimated from the percentage of amorphous and crystalline substances in the composition of chondrites. The estimates obtained are consistent with existing estimates of the age of the solar system.

Incidentally, such a hypothesis of the formation of meteorites allows us to make an interesting assumption regarding the formation of the dusty part of the pre-planet cloud that gave "life" to the planets of the solar system. It is possible that the cloud was initially gas-like, it could contain not only atoms, but also fragments of atoms, ions and fragments of molecules - free radicals, and then a dust component was released from it as a result of collisions and the combination of gas molecules.

In connection with the "cold" hypothesis of the formation of chondritis, another interesting question arises. As you know, there are silicate meteorites and iron meteorites. But no one ever observed a silicate-iron meteorite. Therefore, if the "cold" hypothesis of meteorite formation is true, then the silicate and iron amorphous balls that appeared in the pre-planetary cloud, when colliding with each other, should not stick together.

To verify this assumption, an experiment in a space vacuum in laboratory conditions is necessary. Physicists have learned how to get a vacuum, if not cosmic, then at least close to it. This can be achieved, for example, in this way.

Using a special vacuum pump, air is pumped out of the hermetic vessel to a high degree of rarefaction. But this is not a cosmic vacuum. To achieve it, the so-called cryogenic method is used. Through special ribbed pipes resembling steam heating radiators, liquid hydrogen or helium is passed. The temperature of the pipes drops so much that the air remaining in the chamber freezes and settles on the ribs in the form of hoarfrost.

In a similar chamber, it would be necessary to put the following experience. Direct a beam of iron atoms onto a glass or some other silicate plate and check whether they stick to the surface of the plate. If adhesion occurs at any temperature, this circumstance will prove to be serious evidence against the "cold" hypothesis of the formation of meteorites, because in this case silicate-iron meteorites would have to exist. But if it turned out that coalescence does not take place or occurs only in a certain temperature range, then the "cold" hypothesis of meteorite formation would be well confirmed. Moreover, in a similar way, one could roughly estimate what the temperature in the pre-planet cloud was.