Search academic texts

Information × Registration Number 0219U000241, 0118U004573 , R & D reports Title Astrophysical numerical simulation of the dynamic evolution of stellar systems in galaxies and galactic centre using GRID / GPU GAO cluster popup.stage_title Head Berczik P.P., Registration Date 23-01-2019 Organization Main Astronomical Observatory popup.description2 1.1 We do not observe a strong variation in the age distribution along galactocentric radius. In contrast, the distribution strongly varies along Z-axis. 1.2 The model clusters formed with a high star formation efficiency (SFE) follow a tight mass-dependent relation. However, the low-SFE models present a large scatter in both the "initial" mass and the dissolution time, and a shallower mass-dependent relation than high-SFE clusters and most dissolve within 1 Gyr. 2.1 We analytically derive that the mass fallback rate of the marginally eccentric tidal disruption events can be fatter and slightly higher than the standard fallback rate proportional to t-5/3, whereas it can be fatter and lower for the marginally hyperbolic tidal disruption events. 2.2 We obtain the rate of tidal disruption events to be 4x10-6 yr-1 and estimate the number of objects emitting gravitational waves during the accretion onto the supermassive black hole to be ~230 per Gyr with ~100 of them being possible extreme mass ratio inspirals. 3.1 We find that supermassive black hole binaries coalesce well within one billion years when our models are scaled to galaxies with a steep cusp at low redshift. 3.2 Comparing with previous numerical simulations following the decay of BHs in massive early-type galaxies at z about 3, we confirm that the characteristic density is the most crucial parameter determining the overall BH merging time-scale, despite the structural diversity of the host galaxies. 4. We show that the interaction of the nuclear stellar cluster (NSC) with the gaseous disc (AD) leads to formation of a stellar disc in the central part of the NSC. 5. We find that the three-dimensional R calibration, which uses the N2 and R2 lines, produces reliable abundances in the MaNGA galaxies Product Description popup.authors Іванов Д.Д. Берцик Петер Петерович Велесь Олександр Анатолійович Соболенко М.О. popup.nrat_date 2020-04-02 Close