Gravitational Waves from Inspiralling Compact Binaries in ... - LUTH
Gravitational Waves from Inspiralling Compact Binaries in ... - LUTH Gravitational Waves from Inspiralling Compact Binaries in ... - LUTH
Earlier Work ∗ MBM (1994), Martel Poisson (1999), Pierro et al (2001), Influence of eccentricity on the SNR in GWDA, ∗ Gusev et al (2002), Seto (1991) LISA will be sensitive to eccentric Galactic binary neutron stars and that by measuring their periastron advance, accurate estimates for the total mass of these binaries may be obtained ∗ Damour Schäfer (1987), Schäfer Wex (1994): 2PN GQKR Will Wiseman (1996), Gopakumar Iyer (1997) 2PN GWF, Energy Flux, AM Flux, Evoln of Orbital elts under 2PN GRR ∗ Gopakumar Iyer (2002), 2PN GW Polarisations. Effects of eccentricity, advance of periastron and orbital inclination on power spectrum of the dominant Newtonian part of the polarizations BRI-IHP06-I – p.11/??
Earlier Work ∗ GW from an eccentric binary, during that stage of inspiral where the GRR is so small that the orbital parameters can be treated as essentially unchanging over a few orbital periods (‘adiabatic approx’). ∗ Damour, Gopakumar and Iyer (2004) Analytic method for constructing high accuracy templates for the GW sig- nals from the inspiral phase of compact binaries moving on quasi-elliptical orbits by improved “method of variation of constants” to combine the three time scales involved in the elliptical orbit case, namely, orbital period, periastron pre- cession and radiation reaction time scales, without making the usual approximation of treating the radiative time scale as an adiabatic process. BRI-IHP06-I – p.12/??
- Page 1 and 2: Gravitational Waves from Inspiralli
- Page 3 and 4: Introduction Inspiralling Compact B
- 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: Related Earlier Work ∗ Peters and
- 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 >
- Page 55 and 56: Gauge Invariant Variables < ˙ E3PN
- Page 57 and 58: Hereditary Contributions F 3PN tail
- Page 59 and 60: Log terms in total energy flux Summ
- Page 61 and 62: Log terms in total energy flux FZ t
Earlier Work<br />
∗ MBM (1994), Martel Poisson (1999), Pierro et al (2001),<br />
Influence of eccentricity on the SNR <strong>in</strong> GWDA,<br />
∗ Gusev et al (2002), Seto (1991) LISA will be sensitive to<br />
eccentric Galactic b<strong>in</strong>ary neutron stars and that by<br />
measur<strong>in</strong>g their periastron advance, accurate estimates<br />
for the total mass of these b<strong>in</strong>aries may be obta<strong>in</strong>ed<br />
∗ Damour Schäfer (1987), Schäfer Wex (1994): 2PN GQKR<br />
Will Wiseman (1996), Gopakumar Iyer (1997) 2PN GWF,<br />
Energy Flux, AM Flux, Evoln of Orbital elts under 2PN GRR<br />
∗ Gopakumar Iyer (2002), 2PN GW Polarisations. Effects of<br />
eccentricity, advance of periastron and orbital <strong>in</strong>cl<strong>in</strong>ation<br />
on power spectrum of the dom<strong>in</strong>ant Newtonian part of the<br />
polarizations<br />
BRI-IHP06-I – p.11/??