期刊
ASTROPHYSICAL JOURNAL LETTERS
卷 732, 期 2, 页码 -出版社
IOP PUBLISHING LTD
DOI: 10.1088/2041-8205/732/2/L26
关键词
black hole physics; galaxies: nuclei; gravitational waves
资金
- NAS Ukraine
- Chinese Academy of Sciences [2009S1-5]
- Ministry of Finance [ZDYZ2008-2]
- Volkswagen Foundation [I/80041-043, I/84 678-680]
- Ministry of Science, Research and the Arts of Baden-Wurttemberg) [823.219-439/30, 36]
- EU [RI-508830, RI-031513]
- University of Heidelberg
We investigate a purely stellar dynamical solution to the Final Parsec Problem. Galactic nuclei resulting from major mergers are not spherical, but show some degree of triaxiality. With N-body simulations, we show that equal-mass massive black hole binaries (MBHBs) hosted by them will continuously interact with stars on centrophilic orbits and will thus inspiral-in much less than a Hubble time-down to separations at which gravitational-wave (GW) emission is strong enough to drive them to coalescence. Such coalescences will be important sources of GWs for future space-borne detectors such as the Laser Interferometer Space Antenna (LISA). Based on our results for equal-mass mergers, and given that the hardening rate of unequal-mass binaries is similar, we expect that LISA will see between similar to 10 and similar to few x 10(2) such events every year, depending on the particular massive black hole (MBH) seed model as obtained in recent studies of merger trees of galaxy and MBH co-evolution. Orbital eccentricities in the LISA band will be clearly distinguishable from zero with e greater than or similar to 0.001-0.01.
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