(ed.). Gravitational waves (IOP, 2001)(422s).

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118 LISA: A proposed joint ESA–NASA gravitational-wave missionFigure 10.2. Location of the LISA antenna, 50 000 000 km behind the Earth in orbit aroundthe Sun. The plane of the antenna is tipped at 60 ◦ to the ecliptic.Figure 10.3. Layout of one of the two optical assemblies in each spacecraft. The maincomponents are the optical bench at the centre and the transmit/receive telescope at oneend.optical assemblies in each spacecraft. This is accomplished by supporting thelower part of each optical assembly by a flexure from a common block near thebase of the Y-shaped shield, and the upper part by two adjustable displacement
Description of the LISA mission 119Figure 10.4. Mounting of optical assemblies inside main thermal shield. Each opticalassembly must rotate slowly and smoothly during the year over about a one degree range.Figure 10.5. Optical bench for one optical assembly. Light from the laser is mainly sentout to the telescope, with a little going to the photodiode. Received light from the other endof the arm passes through the beamsplitter to the test mass, and then goes to the photodiode.Changes in the phase of the beat signal determine the changes in the arm length.mechanisms from an arm of the Y, as shown in figure 10.4 (see [10]). Themechanisms provide a very smooth one degree change in the angle between thearms with mainly a one year period.At the centre of each optical bench, shown in figure 10.5 (see [9]), is afreely floating test mass that is protected as much as possible from sources ofspurious accelerations. The basic measurements made by the LISA antenna
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GRAVITATIONAL WAVES
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c IOP Publishing Ltd 2001All righ
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viContents4 Astrophysics of gravita
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viiiContents11.3 Gravitational wave
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xContents16.5 Cosmological perturba
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PrefaceGravitational waves today re
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2 Gravitational waves, theory and e
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10 Gravitational waves, theory and
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SynopsisGravitational waves and the
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Chapter 2Elements of gravitational
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Using the TT gauge to understand gr
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Interaction of gravitational waves
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Analysis of beam detectors 21This d
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Exercises for chapter 2 232. Show t
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Gravitational-wave detectors 25indi
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Gravitational-wave observables 27th
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The physics of interferometers 29
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The physics of interferometers 31Dr
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The physics of interferometers 33Fi
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The physics of resonant mass detect
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The physics of resonant mass detect
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A detector in space 39LISA has been
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Gravitational and electromagnetic w
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Chapter 4Astrophysics of gravitatio
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Sources detectable from ground and
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Variational principles and the ener
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Variational principles and the ener
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Practical applications of the Isaac
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Exercises for chapter 5 57(f)This s
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Expansion for the far field of a sl
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Application of the TT gauge to the
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Page 80 and 81: Application of the TT gauge to the
Page 82 and 83: 6.4.1 Mass-quadrupole radiationEner
Page 84 and 85: Chapter 7Source calculationsNow tha
Page 86 and 87: The r-modes 73As we mentioned in ch
Page 88 and 89: The r-modes 75instability. In an id
Page 90 and 91: The r-modes 77Table 7.1. Gravitatio
Page 92 and 93: The r-modes 79evolution turns out t
Page 94 and 95: ReferencesWe have divided the refer
Page 96 and 97: References 83[19] van der Klis M 19
Page 98 and 99: Solutions to exercises 85For this p
Page 100 and 101: Solutions to exercises 87The gauge
Page 103 and 104: Chapter 8Resonant detectors for gra
Page 105 and 106: Sensitivity and bandwidth of resona
Page 107 and 108: 8.2 Sensitivity for various GW sign
Page 109 and 110: Sensitivity for various GW signals
Page 111 and 112: Recent results obtained with the re
Page 113 and 114: Discussion and conclusions 101Figur
Page 115 and 116: Chapter 9The Earth-based large inte
Page 117 and 118: Introduction 105Figure 9.1. The sim
Page 119 and 120: h(sqrt(1/Hz))10 −610 −810 −10
Page 121 and 122: 18.5 cmThe SA suspension and requir
Page 123 and 124: A few words about the Low Frequency
Page 125 and 126: Conclusion 113Figure 9.7. The R and
Page 127 and 128: Chapter 10LISA: A proposed joint ES
Page 129: Description of the LISA mission 117
Page 133 and 134: Description of the LISA mission 121
Page 145 and 146: Expected gravitational-wave results
Page 161 and 162: References 149[8] Folkner W M 1998
Page 163 and 164: References 151[68] Miralda-Escuda J
Page 165 and 166: Introduction 153detect GWs with a s
Page 167 and 168: Testing theories of gravity 155•
Page 169 and 170: 0Testing theories of gravity 157the
Page 171 and 172: Taking the scalar product we findGr
Page 173 and 174: Gravitational wave radiation in the
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The hollow sphere 169and introduced
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Scalar-tensor cross sections 171mon
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Scalar-tensor cross sections 173Tab
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Scalar-tensor cross sections 175Tab
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References 177Frossati G and Coccia
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Chapter 12Generalities on the stoch
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Introduction 183contribution to the
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Definitions 185The value of H 0 is
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Definitions 18712.2.2 The character
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Definitions 189or, dividing by the
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The overlap reduction function 191O
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The overlap reduction function 193T
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The overlap reduction function 195F
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Achievable sensitivities to the SGW
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Observational bounds 207Table 12.10
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equation gives immediately(ρgwρ
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Chapter 13Sources of SGWBHere we re
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Topological defects 213This correla
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Topological defects 215It can be sh
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Topological defects 217(i)A loop ra
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Topological defects 219• A peak n
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Topological defects 22113.1.2 Hybri
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Inflation 223Hubble radius and when
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Inflation 225as a first approximati
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Inflation 227the lower bound to the
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String cosmology 22913.3 String cos
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String cosmology 231HPre-big bangPo
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String cosmology 233Figure 13.6. h
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First-order phase transitions 23580
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Astrophysical sources 237which is t
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References 239of [71]). However, fo
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References 241[39] Liddle A R 2000
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PART 4THEORETICAL DEVELOPMENTSHerma
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246 Infinite-dimensional symmetries
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Chapter 15Gyroscopes and gravitatio
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270 Gyroscopes and gravitational wa
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Chapter 16Elementary introduction t
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282 Elementary introduction to pre-
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Chapter 17Post-Newtonian computatio
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340 Post-Newtonian computation of b
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PART 5NUMERICAL RELATIVITYEdward Se
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362 Numerical relativityspite of mo
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364 Numerical relativityterms, of m
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366 Numerical relativityHere we hav
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368 Numerical relativityinformation
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370 Numerical relativityThe Palma,
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372 Numerical relativityHyperbolic
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374 Numerical relativityEinstein di
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376 Numerical relativityare the abi
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378 Numerical relativityeach cell i
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380 Numerical relativityFigure 18.1
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382 Numerical relativity1D code [45
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384 Numerical relativityfunctions,
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386 Numerical relativityto a very a
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388 Numerical relativity18.5 Comput
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390 Numerical relativitynumerics an
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392 Numerical relativityinitial dis
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396 Numerical relativityof these re
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400 Numerical relativityof Einstein
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402 Numerical relativity18.9.5.2 Co
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404 Numerical relativity[23] Ashby
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406 Numerical relativity[101] Shapi
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408 Numerical relativity(Singapore:
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410 IndexEhlers Lagrangian, 254Eins
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412 Indexscalarspherical harmonics,
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