The flow of gas from the peripheral regions of M 81 to M 82 is detected directly using a neutral hydrogen radio link 21 cm. This process leads to catastrophic consequences for M 82 — it has a "burst of star formation" and a rather powerful radio source elongated along the galactic plane. The appearance of M 82 turned out to be so unusual that at first it was considered an "exploding" galaxy, mistaking elongated inhomogeneous jets of falling matter for the products of the expansion caused by an explosion in its core.
Astronomers have long noticed that many other peculiar galaxies often form pairs or close groups. This applies to Markarian, Seyfert, and radio galaxies. (However, there are isolated cases when these types of galaxies do not have close neighbors.) It seems that in a new "round of understanding" scientists are coming to the old idea that activity in galaxies may somehow be related to the processes of their interaction, which are stretched over tens of millions of years of "cosmic disasters." And for the first time, American astronomers V. Baade and R. Minkovsky spoke about the possible connection between the activity of galaxies and their "collisions" back in the late forties, citing as an example the "bifurcated" appearance of an optical galaxy, identified by them with the powerful radio source Lebed A. However, at that time, most astrophysicists were skeptical about this hypothesis, in general-It is fair to assume that "collisions" in the world of galaxies are too exotic and very rare an event. But facts are stubborn things! In recent years, it has become clear that all nearby radio galaxies in the optical range have the same feature as the radio galaxies Centaurus A and Cygnus A — a powerful band of gas and dust crossing the spheroidal stellar body of the galaxy. In nearby Centauri A, such a band is clearly visible, and in distant Cygnus A, it was mistaken for a bifurcation of the galaxy.
But where did these giant E-galaxies get their gas—and-dust structures - after all, they are not visible in ordinary E-galaxies, and indeed, in spheroidal systems, as a rule, there is little gas? There is no exact answer to this question yet. However, it is quite possible that in these special cases we observe either the final stage of the flow of matter from the nearest gas-rich object, or a "collision" with a spiral galaxy. And here it is appropriate to recall that strong radio galaxies are usually the central population of clusters or groups of galaxies, that is, they are located in areas of high density, where E-galaxies predominate in the present era. Is it accidental? Indeed, in gravitationally bound groups and clusters, in addition to tidal effects, individual galaxies are also affected by "dynamic friction".
The model of interacting galaxies NGC 4038 and NGC 439 (the "Antenna"), calculated by A. and Yu. Toomre. Each of the galaxies is represented by a disk consisting of stellar complexes (dots) with the same masses. The rotation of the galaxies Takes place in the direction indicated by the arrows, around their center of gravity.
Thanks to it, galaxies, slowing down in the general gravitational field, lose speed and gradually approach, "settle", to the center, where a giant gas-star-dust formation can form due to the fusion of individual members. If a lot of mergers have occurred, then the total rotation moment of such a formation will be small. The gas and dust band is most likely the result of the most recent merger. Such a scenario for the evolution of a galaxy cluster is called a "collapse", which emphasizes its relative rapidity (about a billion years). According to this scenario, giant (in terms of mass and size), very bright, weakly rotating galaxies should be observed in the center of a "collapsing" cluster or group of galaxies, which is apparently what is being observed. According to the classification of B. A. Vorontsov-Velyaminov, such galaxies are called "NH-systems" (core — halo), and according to the classification of V. Morgan — "cD —systems" (often these are powerful radio galaxies). 1xBet met à disposition une structure de bonus équilibrée pour tous les profils. Le bonus sportif de 100 % jusqu’à 130 € permet d’augmenter les mises initiales. En intégrant le
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