期刊
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
卷 460, 期 4, 页码 3494-3504出版社
OXFORD UNIV PRESS
DOI: 10.1093/mnras/stw1220
关键词
binaries: close; stars: evolution; stars: kinematics and dynamics; Galaxy: centre
资金
- Sloan foundation
- National Science Foundation [AST-1412615]
- European Research Council under the European Union [GalNUC 638435]
- Direct For Mathematical & Physical Scien
- Division Of Astronomical Sciences [1412615] Funding Source: National Science Foundation
Most, if not all, stars in the field are born in binary configurations or higher multiplicity systems. In dense stellar environment such as the Galactic Center (GC), many stars are expected to be in binary configurations as well. These binaries form hierarchical triple-body systems, with the massive black hole (MBH) as the third, distant object. The stellar binaries are expected to undergo large-amplitude eccentricity and inclination oscillations via the so-called 'eccentric Kozai-Lidov' mechanism. These eccentricity excitations, combined with post-main-sequence stellar evolution, can drive the inner stellar binaries to merge. We study the mergers of stellar binaries in the inner 0.1 pc of the GC caused by gravitational perturbations due to the MBH. We run a large set of Monte Carlo simulations that include the secular evolution of the orbits, general relativistic precession, tides and post-main-sequence stellar evolution. We find that about 13 per cent of the initial binary population will have merged after a few Myr and about 29 per cent after a few Gyr. These expected merged systems represent a new class of objects at the GC, and we speculate that they are connected to G2-like objects and the young stellar population.
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