Journal
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
Volume 484, Issue 3, Pages 3279-3290Publisher
OXFORD UNIV PRESS
DOI: 10.1093/mnras/stz208
Keywords
black hole physics; stars: kinematics and dynamics; pulsars: general
Categories
Funding
- Ministry of Defense and Aerospace Industry of the Republic of Kazakhstan [BR05336383]
- German Research Foundation (DFG) [Sonderforschungsbereich SFB 881]
- Alexander von Humboldt Foundation
- Federal Ministry for Education and Research
- National Science Foundation of China (NSFC) [11673032]
- Strategic Priority Research Program (Pilot B) 'Multi-wavelength gravitational wave universe' of the Chinese Academy of Sciences [XDB23040100]
- China-Kazakhstan international cooperation project of Chinese Academy of Sciences (CAS) 'Evolution of star clusters in galactic nuclei with supermassive black holes and central accretion disks' [114A11KYSB20170015]
- President's International Fellowship for Visiting Scientists program of CAS
- Volkswagen Foundation (VW) under the Trilateral Partnerships [90411]
- project GRACE 2: 'Scientific simulations using programmable hardware' (VW) [I84678/84680]
- Gauss Centre for Supercomputing (GSC) e.V.
- International Space Science Institute, Bern, Switzerland [393]
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We study the dynamics and evolution of the Milky Way nuclear star cluster performing a high-resolution direct one-million-body simulation. Focusing on the interactions between such stellar systems and the central supermassive black hole, we find that different stellar components adapt their overall distribution differently. After 5 Gyr, stellar mass black holes are characterized by a spatial distribution with power-slope -1.75, fully consistent with the prediction of Bahcall-Wolf pioneering work. Using the vast amount of data available, we infer the rate for tidal disruption events, being 4 x 10(-6) per yr, and estimate the number of objects that emit gravitational waves during the phases preceding the accretion on to the super-massive black hole, similar to 270 per Gyr. We show that some of these sources could form extreme mass-ratio inspirals. We follow the evolution of binary stars population, showing that the initial binary fraction of 5 per cent drops down to 2.5 per cent inside the inner parsec. Also, we explored the possible formation of binary systems containing a compact object, discussing the implications for millisecond pulsars formation and the development of Ia Supernovae.
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