How galaxy collisions can avoid huge black holes

Conflicts between galaxies were thought to increase the activity of giant black holes in their centers. However, researchers have developed a number of precise simulations of multiple collisions, some of which may reduce the movement of their central black holes. The reason is that certain headaches can actually clean up the black holes in the galaxy’s fuel.

When you think of galaxies colliding with galaxies, it may be tempting to imagine that there is such a thing as a cosmic accident, such as the explosion of stars exploding and exploding. But in reality it is close to a pair of clouds, often taking the largest and the smallest. It is unthinkable that any of the stars in them would clash. This means that when galaxies collide, the consequences can be devastating.

It is drawn from the galaxy nucleus gas

Artist’s Opinion on the Gap from the Galaxy Nucleus Credit: © 2021 Miki et al.

Galaxyes collide in different ways. Sometimes small galaxies collide with a large unit or pass or merge many stars along the way. But galaxies can also collide in front of each other, splitting the big one into waves and splitting the two smaller ones. It is at this point that something exciting happens in the galactic nucleus.

“In the heart of most galaxies there is something huge Black hole, Or MHH, ”says Yohi Mickey, a research fellow at the University of Tokyo. “As long as astronomers explore galaxy collisions, it is estimated that a collision will always lead to MBH fuel in the nucleus. And this fuel nourishes the MBA, significantly increases its activity, and we see, among other things, ultraviolet and X-ray light. However, we now have good reason to believe that this series of events is inevitable and that the opposite can sometimes be true. ”

Dynamic Model Galaxy Conflicts

The dynamic model is visualized by simulating two different conditions. The top row shows the main activity of the conflict reduction, the bottom row shows the main activity that increases the conflict. Credit: © 2021 Miki et al.

It seems logical that galaxy collisions will only increase MBH activity, but Mickey and the team were eager to test that thinking. Make detailed models of galaxy collisions and run them on supercomputers. The team is pleased that in some cases, the smaller galaxy has been able to unravel the larger issue around the MBH. This reduces rather than increases activity.

Mickey’s “B” around the “B” in the “X” “” “” “” “” “” “” “” “” “” “” “” “” “” “” “” “” “” ” »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» » »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» » »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» »» » MHH in Torus, or We have completed the dynamic transformation of the gas element around the donut. These events could last for millions of years, although we are still not sure how long the MBH movement will last.

This research can help us understand our own evolution Milky Way. Astronomers are convinced that our galaxy has already collided with many smaller ones.


Visual dynamic model simulating the main movement of conflict resolution. Credit: © 2021 Miki et al.

Reference: “Loss of Central Black Hole Gas Storage by Galaxy Conflicts” by Yohi Mickey, Masao Morei and Toshihiro Kawaguchi, January 25, 2021; Nature astronomy.
Doy: 10.1038 / s41550-020-01286-9

This work is partially supported by a grant for special support research in Education, Culture, Sports, Science and Technology (MEXT) (16002003), Japanese Community for Science Research in Support of Science Promotion (JSPS) ((S) 20224002; (A) 21244013; (C) JP17K05389), JSPS KAKENHI grant numbers JP20K14517 and JP20K04022 and the NAOJ Research Coordinating Committee (20DS-0502).

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