Gravitational Waves from Inspiralling Compact Binaries in ... - LUTH
Gravitational Waves from Inspiralling Compact Binaries in ... - LUTH Gravitational Waves from Inspiralling Compact Binaries in ... - LUTH
Eccentric Binaries Based on Koenigdorffer and Gopakumar Stellar-mass compact binaries in eccentric orbits are excellent sources for LISA. LISA will “hear” GW from intermediate-mass black holes moving in highly eccentric orbits K. Gültekin, M. C. Miller, and D. P. Hamilton (2005), T. Matsubayashi, J. Makino, and T. Ebisuzaki (2005), M. A. Gürkan, J. M. Fregeau, and F. A. Rasio (2005) Several papers indicate that SMBHB formed from galactic mergers, may coalesce with orbital eccentricity S. J. Aarseth (2003), P. Berczik, D. Merritt, R. Spurzem, and H.-P. Bischof (2006), O. Blaes, M. H. Lee, and A. Socrates( 2002), P. J. Armitage and P. Natarajan (2005), M. Iwasawa, Y. Funato, and J. Makino (2005) These investigations employ different techniques and astrophysical scenarios to reach the above conclusion. BRI-IHP06-I – p.3/??
Kozai Mechanism One proposed astrophysical scenario, involves hierarchical triplets modeled to consist of an inner and an outer binary. If the mutual inclination angle between the orbital planes of the inner and of the outer binary is large enough, then the time averaged tidal force on the inner binary may induce oscillations in its eccentricity, known in the literature as the Kozai mechanism Kozai (1962),M. C. Miller and D. P. Hamilton (2002), E. B. Ford, B. Kozinsky, and F. A. Rasio (2000), Wen (2003) BRI-IHP06-I – p.4/??
- Page 1 and 2: Gravitational Waves from Inspiralli
- Page 3: Introduction Inspiralling Compact B
- Page 7 and 8: Kozai Mechanism, Globular Clusters
- Page 9 and 10: Kicks, Eccentricity Compact binarie
- Page 11 and 12: Related Earlier Work ∗ Peters and
- Page 13 and 14: Earlier Work ∗ GW from an eccentr
- Page 15 and 16: FF as fn of initial eccentricity e0
- Page 17 and 18: Eccentric Signal Plots of s(t) (up
- Page 19 and 20: The Generation Modules Generation p
- Page 21 and 22: Present Work Represent GW from a bi
- Page 23 and 24: PN order of Multipoles For a given
- Page 25 and 26: Radiative moments - Source moments
- Page 27 and 28: 3PN EOM for ICB a i = dvi dt AE = 1
- Page 29 and 30: Instantaneous Terms dE dt inst d
- Page 31 and 32: 3PN Instantaneous Terms dE dt 2PN
- Page 33 and 34: Transfn of World lines Having obtai
- Page 35 and 36: Energy Flux - Modified Harmonic Coo
- Page 37 and 38: 3PN generalised Quasi-Keplerian rep
- Page 39 and 40: 3PN generalised Quasi-Keplerian rep
- Page 41 and 42: 3PN GQKR - Mhar n = (−2E) 3/2 +11
- Page 43 and 44: 3PN GQKR - Mhar + Φ = 2 π 70 16
- Page 45 and 46: Orbital average - Energy flux -MHar
- Page 47 and 48: Orbit Averaged Energy Flux - MHar <
- Page 49 and 50: Comments Note: No term at 2.5PN. 2.
- Page 51 and 52: Comments Useful internal consistenc
- Page 53 and 54: Gauge Invariant Variables < ˙ E >
Kozai Mechanism<br />
One proposed astrophysical scenario, <strong>in</strong>volves hierarchical<br />
triplets modeled to consist of an <strong>in</strong>ner and an outer b<strong>in</strong>ary. If<br />
the mutual <strong>in</strong>cl<strong>in</strong>ation angle between the orbital planes of<br />
the <strong>in</strong>ner and of the outer b<strong>in</strong>ary is large enough, then the<br />
time averaged tidal force on the <strong>in</strong>ner b<strong>in</strong>ary may <strong>in</strong>duce<br />
oscillations <strong>in</strong> its eccentricity, known <strong>in</strong> the literature as the<br />
Kozai mechanism<br />
Kozai (1962),M. C. Miller and D. P. Hamilton (2002), E. B. Ford, B. Koz<strong>in</strong>sky, and F. A. Rasio (2000), Wen (2003)<br />
BRI-IHP06-I – p.4/??
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