Milky Way galaxies are thought to have merged and attracted smaller galaxies and groups of stars, making these alien stars their own. In some cases, mergers were as recent as we could find a body free of matter before us, a group of stars orbiting together in the Milky Way. But over time, the interaction with the rest of the Milky Way galaxy will gradually destroy any of the structures in the Snow House.
Therefore, it is surprising that scientists have discovered the remains of a balloon on some of the oldest stars. This finding is consistent with the galaxy model of “growth through synthesis”, but raises questions about how mass-intensive it can be.
Gaya Data Mining
The results began with an analysis of data from the European Space Agency Misija Gaya, Which aims to create a map of the bird’s path in at least three dimensions. Gaya has photographed about a billion objects dozens of times, which is enough to estimate their position and motion around the heart of the Milky Way. This map has helped scientists to identify structures in our galaxy that are not only physically close to each other, but that there are many galaxies moving in the same direction.
Gaia data mining is very useful for this type of structure, as defined by the software algorithm STREAMFINDER. The program made it possible to detect the flow of C – 19 stars as a group of stars move together through the Milky Way’s halo.
One way to check if these star groups actually appeared as part of a group is to check their age. Clusters often contain stars of the same age. One way to find out if stars are forming at the same time is to examine the heavier elements. At the time of the Big Bang, there were fewer elements heavier than helium, so most of the heavier elements now in existence belong to previous stars. Later in the history of the universe a star is formed, and the star is more likely to have these heavier elements.
(Astronomers call helium any element heavier than metal, and stars call the amount of solid elements metal. However, this is likely to confuse most non-astronomers, so we will avoid it.)
Thus, the astronomers in the new work measured the amount of heavier elements in the stars that are thought to be in the C – 19 stream. With the exception of one organ, they were all identical, indicating that the flow was actually a fragile remnant of the group. However, the results were also surprising: very small amounts of heavy elements.
Ancient history
The most common method of recording heavy elements is the ratio of iron (which forms only at the end of the life of a giant star) to hydrogen. Hydrogen has always been the most abundant element in the universe, and iron levels have been steadily rising over time. Thus the higher the ratio of iron to hydrogen, the more the star formed.
In the case of C-19 flow, the ratio was very low. The formation of the C-19 stars is very low, about 3 billion years after the Big Bang or when the universe was only a quarter of its current age. It is possible that they formed a little earlier.
Within the Bird Trail, hundreds of stars with similar low-weight elements have been identified. But I have never seen a cluster of all the players at such a low level. In fact, prior to this discovery, the Milky Way clusters were thought to contain heavier Earth elements, all at higher levels than the C-19 stream. This was true despite the fact that based on the distribution of known groups, we expect five levels with heavier elements similar to those in the C-19 stream.
The absence of other groups indicates that most of the early groups like this stream were already disturbed and disappeared in the background of the stars in the Milky Way. This raises the question of why the C-19 does not have traffic. This is especially unexpected as the orbit of the electric current around the core of the galaxy carries it deeper into the Milky Way, giving it ample opportunity to interact with other features that need to be turned off.
One possible explanation is that the group entered the Milky Way as part of a swallowed dwarf galaxy. The structure of the dwarf galaxy will provide some protection until it collapses, and its stars will scatter on BirdTake. If so, the mass that caused C-19 to flow was a large fraction of the stars in the dwarf galaxy at the time.
Whatever it explains, the presence of the C-19 stream tells us things about the history of the universe. The authors conclude: “The very presence of C – 19 proves that spherical clusters must have formed in the low-mineral environment in which the first galaxy structures were to accumulate.”
Ganta, 2022 m DOI: 10.1038 / s41586-021-04162-2 (About DOI).
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