Astronomers have been trying to understand the formation of binary stars for a long time. The most important thing was to understand how mass affects the multiplicity. I had to analyze a lot of young stars in molecular clouds, as well as look for effects that affect the process.
The problem is that between the stars there are dynamic mechanisms that lead to the fact that one is pushed out or they are ways to attract another one to them. Some data said that young stars are more likely to occur in pairs. But there was nothing more to say, because few objects were checked.
Scientists decided to rectify the situation and tracked the “youth” in the Perseus cloud. A submillimeter survey was used to examine the dense natal material of the nucleus around the stars, and 24 star systems were determined. It turned out that most of the binaries are near the center of the dust cores, which means they are still young enough to escape and retire. Approximately half resides in elongated main structures. Models show that all the stars are formed in pairs, but then they move away due to the release, or the connection between them becomes closer. The main conclusion is that each dust core is the place where two stars appear at once, and not one.
