Gravitational Waves from Inspiralling Compact Binaries in ... - LUTH
Gravitational Waves from Inspiralling Compact Binaries in ... - LUTH Gravitational Waves from Inspiralling Compact Binaries in ... - LUTH
Method of variation of constants First construct soln to the ‘unperturbed’ system, defined by ˙x = v , ˙v = A0(x, v). The solution to the exact system ˙x = v , ˙v = A(x, v) , obtained by varying the constants in the generic solutions of the unperturbed system. The method assumes ( true for A conservative 2P N or Aconservative 3P N ) that the unperturbed system admits sufficiently many integrals of motion to be integrable. E.g. if A0 = A2P N, we have four first integrals: the 2PN accurate energy and 2PN accurate angular momentum of the binary written in the 2PN accurate center of mass frame as c1 and ci BRI-IHP06-I – p.102/?? 2:
Method of variation of constants c1 = E(x1, x2, v1, v2)|2(3)PN CM , c i 2 = Ji(x1, x2, v1, v2)|2(3)PN CM , Vectorial structure of c i 2, indicates that the unperturbed motion takes place in a plane. Problem is restricted to a plane even in the presence of radiation reaction. Introduce polar coordinates in the plane of the orbit r and φ such that x = i r cos φ + j r sin φ with, i = p, j = q cos i + N sin i. Functional form for the solution to the unperturbed equations of motion may be expressed as r = S(l; c1, c2) ; ˙r = n ∂S ∂l (l; c1, c2) , φ = λ + W (l; c1, c2) ; ˙ φ = (1 + k)n + n ∂W ∂l (l; c1, c2) , where λ and l are two basic angles, which are 2π periodic and c2 = |c i 2|. BRI-IHP06-I – p.103/??
- 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
- Page 63 and 64: Complete 3PN energy flux - Mhar <
- Page 65 and 66: Complete 3PN energy flux - Mhar <
- Page 67 and 68: Present Work Extends the circular o
- Page 69 and 70: Angular Momentum Flux Hereditary co
- Page 71 and 72: Far Zone Angular Momentum Flux dJi
- Page 73 and 74: Far Zone Angular Momentum Flux dJi
- Page 75 and 76: 3PN AMFlux - Shar dJi dt dJi dt
- Page 77 and 78: Orbital Averaged AMF - ADM Using th
- Page 79 and 80: Orbital Averaged AMF - ADM 〈 dJ d
- Page 81 and 82: Orbital Averaged AMF - ADM 〈 dJ d
- Page 83 and 84: Evoln of orbital elements under GRR
- Page 85 and 86: Evoln of orbital element n under GR
- Page 87 and 88: Evoln of orbital element n under GR
- Page 89 and 90: Evoln of orbital element et under G
- Page 91 and 92: Evoln of orbital element ar under G
- Page 93 and 94: Evoln of orbital element ar under G
- Page 95 and 96: PART II Based on Phasing of Gravita
- Page 97 and 98: Beyond Orbital Averages Going beyon
- Page 99 and 100: Phasing of GWF TT radn field is giv
- Page 101 and 102: Phasing of GWF Orbital phase = φ,
- Page 103: Method of variation of constants A
- 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 and 152: h+(t) and h×(t) Scaled h + (t) Sca
- Page 153 and 154: ¯n/ni and ñ/n ēt and ˜et versus
Method of variation of constants<br />
First construct soln to the ‘unperturbed’ system, def<strong>in</strong>ed by<br />
˙x = v ,<br />
˙v = A0(x, v).<br />
The solution to the exact system<br />
˙x = v ,<br />
˙v = A(x, v) ,<br />
obta<strong>in</strong>ed by vary<strong>in</strong>g the constants <strong>in</strong> the generic solutions of<br />
the unperturbed system. The method assumes ( true for<br />
A conservative<br />
2P N<br />
or Aconservative 3P N ) that the unperturbed system<br />
admits sufficiently many <strong>in</strong>tegrals of motion to be <strong>in</strong>tegrable.<br />
E.g. if A0 = A2P N, we have four first <strong>in</strong>tegrals: the 2PN<br />
accurate energy and 2PN accurate angular momentum of<br />
the b<strong>in</strong>ary written <strong>in</strong> the 2PN accurate center of mass frame<br />
as c1 and ci BRI-IHP06-I – p.102/??<br />
2: