期刊
PHYSICAL REVIEW D
卷 77, 期 8, 页码 -出版社
AMER PHYSICAL SOC
DOI: 10.1103/PhysRevD.77.081502
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资金
- Direct For Mathematical & Physical Scien
- Division Of Physics [0914553, GRANTS:13826084] Funding Source: National Science Foundation
- Direct For Mathematical & Physical Scien
- Division Of Physics [0925345] Funding Source: National Science Foundation
We present results from numerical relativity simulations of equal-mass, nonspinning binary-black-hole inspirals and mergers with initial eccentricities e <= 0.8 and coordinate separations D >= 12M of up to 9 orbits (18 gravitational wave cycles). We extract the mass M-f and spin a(f) of the final black hole and find, for eccentricities e less than or similar to 0.4, that a(f)/M-f approximate to 0.69 and M-f/M-adm approximate to 0.96 are independent of the initial eccentricity, suggesting that the binary has circularized by the merger time. For e greater than or similar to 0.5, the black holes plunge rather than orbit, and we obtain a maximum spin parameter a(f)/M-f approximate to 0.72 around e = 0.5.
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