Gravitational Waves from Inspiralling Compact Binaries in ... - LUTH
Gravitational Waves from Inspiralling Compact Binaries in ... - LUTH Gravitational Waves from Inspiralling Compact Binaries in ... - LUTH
h+(t) and h×(t) The plots for the scaled h+(t) and h×(t) (Newtonian in amplitude and 3.5PN in orbital motion) as functions of l/(2π). The slow chirping and the amplitude modulation due to the periastron precession are clearly visible in the two upper panels. In the two bottom panels, we zoom into the initial stages of the orbital evolution in order to show the effect of the periodic orbital motion and the periastron advance on the scaled h+(t) and h×(t). The initial and final values of the relevant orbital elements are marked on top of the plots. The panels are plotted for a binary consisting of equal masses, so that η = 0.25, and the orbital inclination angle is given by i = π/3. The orbital evolution is terminated when j = √ 48. BRI-IHP06-I – p.150/??
¯n/ni and ñ/n ēt and ˜et versus l/(2π) BRI-IHP06-I – p.151/??
- Page 101 and 102: Phasing of GWF Orbital phase = φ,
- Page 103 and 104: Method of variation of constants A
- Page 105 and 106: Method of variation of constants c1
- Page 107 and 108: Method of variation of constants At
- Page 109 and 110: Method of variation of constants An
- Page 111 and 112: Method of variation of constants Al
- Page 113 and 114: Method of variation of constants Fo
- Page 115 and 116: Method of variation of constants Du
- Page 117 and 118: Implementation Compute 3PN accurate
- Page 119 and 120: 3PN accurate conservative dynamics
- Page 121 and 122: 3PN accurate conservative dynamics
- Page 123 and 124: 3PN accurate conservative dynamics
- Page 125 and 126: 3PN accurate conservative dynamics
- Page 127 and 128: 3PN accurate conservative dynamics
- Page 129 and 130: 3.5PN accurate reactive dynamics A
- Page 131 and 132: 3.5PN accurate reactive dynamics Fi
- Page 133 and 134: 3.5PN accurate reactive dynamics dc
- Page 135 and 136: 3.5PN accurate reactive dynamics 4
- Page 137 and 138: Secular variations d¯n dt dēt dt
- Page 139 and 140: Periodic variations To complete thi
- Page 141 and 142: Periodic variations One can analyti
- Page 143 and 144: Periodic variations ˜cl = − 2ξ5
- Page 145 and 146: Periodic variations Above results m
- Page 147 and 148: Periodic variations ˜ l(l; ¯ca) =
- Page 149 and 150: ¯n/ni and ñ/n versus l/(2π) n /
- Page 151: h+(t) and h×(t) Scaled h + (t) Sca
- Page 155 and 156: ¯cl and ˜cl ¯cλ and ˜cλ versu
- Page 157 and 158: Validity of Results Circular orbits
- Page 159: References 1. P. C. Peters, Phys. R
h+(t) and h×(t)<br />
The plots for the scaled h+(t) and h×(t) (Newtonian <strong>in</strong><br />
amplitude and 3.5PN <strong>in</strong> orbital motion) as functions of l/(2π).<br />
The slow chirp<strong>in</strong>g and the amplitude modulation due to the<br />
periastron precession are clearly visible <strong>in</strong> the two upper<br />
panels. In the two bottom panels, we zoom <strong>in</strong>to the <strong>in</strong>itial<br />
stages of the orbital evolution <strong>in</strong> order to show the effect of<br />
the periodic orbital motion and the periastron advance on<br />
the scaled h+(t) and h×(t). The <strong>in</strong>itial and f<strong>in</strong>al values of the<br />
relevant orbital elements are marked on top of the plots. The<br />
panels are plotted for a b<strong>in</strong>ary consist<strong>in</strong>g of equal masses, so<br />
that η = 0.25, and the orbital <strong>in</strong>cl<strong>in</strong>ation angle is given by<br />
i = π/3. The orbital evolution is term<strong>in</strong>ated when j = √ 48.<br />
BRI-IHP06-I – p.150/??
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