MG15 - Talk detail |
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Participant |
RASTELLO, SARA | |||||||
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Institution |
SAPIENZA, UNIVERSITY OF ROME - PIAZZALE ALDO MORO 5 - ROME - ITALY - Italy | |||||||
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Session |
GW8 |
Accepted |
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Talk |
Oral abstract |
Title |
Stellar Black Hole Binary mergers in Open Clusters | |||||
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Abstract |
I will present the results of our work on black hole binary (BHB) mergers in low dense star cluster. We perform a suite of direct-summation N−body simulations of small-and intermediate-size open clusters. These clusters host BHBs with masses in the range of the first LIGO/Virgo detections. For some of our models the binaries become very hard. Some of them are retained in the cluster and merge there, while ejected binaries typically have associated merger timescales which are too long. We find that perturbing stars around BHB systems are key to their coalescence, which would exceed a Hubble time if they were isolated. Those which merge in the cluster can be detected with an elapsed time of a few years with both ground-based detectors and space-borne ones, such as LISA, because they have a relatively high eccentricity. We estimate the BHB merger rate to be of R_mrg ∼ 2 yr^ −1 Gpc^ −3 . |
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Session |
GW8 |
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Time |
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Talk |
Poster abstract |
Title |
The secular evolution of the Nuclear Star Cluster of the Milky Way. | |||||
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Abstract |
Nuclear Stellar Clusters are so dense stellar systems (up to 10^7 stars in few parsec radius) that their dynamics cannot be followed with the high precision, direct summation available N-body codes over a long integration time. This poster introduces the main idea of our project, that is of studying the dynamics of the MW NSC by means of a new approach to work in a direct summation code. The focus is on setting an inner region of the MW NSC containing a ”treatable” number of stars (10^5 to 10^6 stars) where we run the direct N-body simulation with the advanced code NBODY6++GPU while modeling the region surrounding the subset sphere ”boundary” by a suitable method preserving precision and speed. This strategy will allow us to study the evolution of the NSC over its 2-body relaxation time with an acceptable numerical effort by mean of a massive computational platform. |
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Pdf file |
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