On May 29 at 11 a.m. in the Round Hall of the Institute there will be a seminar by Marina Viktorovna Ishchenko (MAO NASU, FAI) on the topic: “The Triune Model of the Dynamic Evolution of the Galactic Center on the Cosmological Time Scale”. The seminar will be held in off-line format. FAI researchers and specialists from other institutions working in this field are invited.

The report will be devoted to studying the dynamic evolution of globular clusters (GCs) using the method of direct N-body modelling over 10 billion years ago. To be more motivated by the physics of past Galactic evolution, we integrated into our code models of Milky Way-like variable gravitational potential that we selected from the IllustrisTNG-100 cosmological database. Thus, the evolution of the Galaxy has a smoothed distribution of the mass of the disk and halo over time, as well as the corresponding sizes.
The report will present three main results.
1. Analysis of the evolution of the orbits of 160 CS over 10 billion years, considering the dynamic potential. The estimation of orbital parameters, distribution in the Galaxy, and the evolution of angular momentum will also be presented.
2. A selection of clusters will be presented that, during their evolution, have close passages (up to 100 pc) from the Galactic centre. Let us estimate the number of such passages and their physical characteristics (mutual distance and flight speed).
3. We will analyze in detail the close interaction between the CSs themselves in the Galaxy. We will consider close passages if the mutual distance from the centres of clusters is at most their two sums of masses of half radii. Let us estimate the probability of collisions between them and determine the regions in the Galaxy where such collisions (close passages with each other) are most likely.

Articles on which the report is based:
Milky Way globular clusters on cosmological timescales I. Evolution of the orbital parameters in time-varying potentials
Milky Way globular clusters on cosmological timescales II. Interaction with the Galactic centre
Milky Way globular clusters on cosmological timescales III. Interaction rates