Gravitational Waves from Inspiralling Compact Binaries in ... - LUTH
Gravitational Waves from Inspiralling Compact Binaries in ... - LUTH Gravitational Waves from Inspiralling Compact Binaries in ... - LUTH
PART I Based on 3PN Gravitational wave fluxes of energy and angular momentum from inspiralling eccentric binaries K. Arun, L. Blanchet, B. R. Iyer and M. S. S. Qusailah Part I, II, III (2006) - To be submitted
Introduction Inspiralling Compact Binaries (ICB) are considered to be the most probable sources of detectable gravitational radiation for laser interferometric gravitational-wave detectors. ICB are usually modeled as point particles in quasi-circular orbits. For long lived compact binaries, the quasi-circular approximation is quite appropriate. Gravitational Radiation Reaction (GRR) decreases the orbital eccentricity to negligible values by the epoch the emitted gravitational radiation enters the sensitive bandwidth of the interferometers. For a lower cutoff of 40 Hz, the binary enters detector when orbital freq is 20 HZ. For NS-NS binary corresponds to orbital radius of 290 km and orbital vel .12c For an isolated binary, the eccentricity goes down roughly by a factor of three, when its semi-major axis is halved since e/e0 = (a/a0) 19/12 - (Peters, 64) BRI-IHP06-I – p.2/??
- Page 1: Gravitational Waves from Inspiralli
- Page 5 and 6: Kozai Mechanism One proposed astrop
- 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
PART I<br />
Based on<br />
3PN <strong>Gravitational</strong> wave fluxes of energy and angular<br />
momentum <strong>from</strong> <strong>in</strong>spirall<strong>in</strong>g eccentric b<strong>in</strong>aries<br />
K. Arun, L. Blanchet, B. R. Iyer and<br />
M. S. S. Qusailah<br />
Part I, II, III (2006) - To be submitted
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