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Gravitational Waves, pack: Volumes 1 and 2: Volume 1: Theory and Experiment, Volume 2: Astrophysics and Cosmology [Multiple-component retail product]

(Professor, Department of Theoretical Physics, University of Geneva, Switzerland)
  • Formatas: Multiple-component retail product, 1328 pages, aukštis x plotis x storis: 252x194x78 mm, weight: 3412 g
  • Išleidimo metai: 05-Apr-2018
  • Leidėjas: Oxford University Press
  • ISBN-10: 0198755287
  • ISBN-13: 9780198755289
Kitos knygos pagal šią temą:
Gravitational Waves, pack: Volumes 1 and 2: Volume 1: Theory and Experiment, Volume 2: Astrophysics and CosmologyDidesnis paveikslėlis
  • Formatas: Multiple-component retail product, 1328 pages, aukštis x plotis x storis: 252x194x78 mm, weight: 3412 g
  • Išleidimo metai: 05-Apr-2018
  • Leidėjas: Oxford University Press
  • ISBN-10: 0198755287
  • ISBN-13: 9780198755289
Kitos knygos pagal šią temą:
Pastovi nuoroda: https://www.kriso.lt/db/9780198755289.html
Raktažodžiai:
The two-volume book Gravitational Waves provides a comprehensive and detailed account of the physics of gravitational waves. While Volume 1 is devoted to the theory and experiments, Volume 2 discusses what can be learned from gravitational waves in astrophysics and in cosmology, by systematizing a large body of theoretical developments that have taken place over the last decades. The second volume also includes a detailed discussion of the first direct detections of gravitational waves. In the author's typical style, the theoretical results are generally derived afresh, clarifying or streamlining the existing derivations whenever possible, and providing a coherent and consistent picture of the field.

The first volume of Gravitational Waves, which appeared in 2007, has established itself as the standard reference in the field. The scientific community has eagerly awaited this second volume. The recent direct detection of gravitational waves makes the topics in this book particularly timely.

Recenzijos

The book covers a staggering breadth of material and is extremely useful as a bird's-eye overview of the field... From now on I will recommend it as the best entry point for students who want to join this blooming research field. * Emanuele Berti, Physics Today * 'The presentation of the material, including the notation and layout, is very clear. The book is written at a level that will appeal to advanced students and active researchers. [ ...] The book clearly fills a gap in the literature. It deserves to become a standard textbook in gravitation and to be on the book-shelf of everybody who is seriously interested in gravitational wave astronomy.' * General Relativity and Gravitation * 'The need for a textbook that treats the production and detection of GWs systematically is clear. Michele Maggiore has succeeded in doing this in a way that is fruitful not only for the young physicist starting to work in the field, but also for the experienced scientist needing a reference book for everyday work. ' * CERN Courier * 'For its comprehensive coverage of the theoretical and experimental aspects of gravitational waves, and for the high quality of its writing, this book is a truly remarkable achievement. I recommend it with great enthusiasm to anyone interested in this exciting topic.' * Classical and Quantum Gravity * 'Students and experienced researchers will welcome Michele Maggiore's timely and authoritative new text book. ' * Nature * 'A very good book, and it fills a gap in the literature. [ ...] It is an ideal textbook for a monographic introductory course on gravitational waves, for graduates or advanced undergraduates, [ and] it could also be the basic reference text for researchers, both experimentalists and theoreticians. ' * The Gravitational Voice * '...excellent and useful material...on an important new frontier of astronomy and of fundamental physics. I look forward to Volume 2, and even more so to the dawn of gravitational-wave astronomy. ' * Nature * I would recommend this text to anyone who is interested in gravitational waves. * Kymani Armstrong-Williams, Physics Book Reviews *

Gravitational Waves: Volume 1: Theory and Experiments
Notation
xvi
Part I: Gravitational-wave theory
1(332)
1 The geometric approach to GWs
3(49)
1.1 Expansion around flat space
4(3)
1.2 The transverse-traceless gauge
7(6)
1.3 Interaction of GWs with test masses
13(13)
1.3.1 Geodesic equation and geodesic deviation
13(2)
1.3.2 Local inertial frames and freely falling frames
15(2)
1.3.3 TT frame and proper detector frame
17(9)
1.4 The energy of GWs
26(14)
1.4.1 Separation of GWs from the background
27(2)
1.4.2 How GWs curve the background
29(6)
1.4.3 The energy-momentum tensor of GWs
35(5)
1.5 Propagation in curved space-time
40(8)
1.5.1 Geometric optics in curved space
42(4)
1.5.2 Absorption and scattering of GWs
46(2)
1.6 Solved problems
48(3)
1.1 Linearization of the Riemann tensor in curved space
48(1)
1.2 Gauge transformation of hμupsilon and R(1)μupsilonρσ
49(2)
Further reading
51(1)
2 The field-theoretical approach to GWs
52(49)
2.1 Linearized gravity as a classical field theory
53(13)
2.1.1 Noether's theorem
53(5)
2.1.2 The energy-momentum tensor of GWs
58(3)
2.1.3 The angular momentum of GWs
61(5)
2.2 Gravitons
66(15)
2.2.1 Why a spin-2 field?
66(4)
2.2.2 The Pauli-Fierz action
70(4)
2.2.3 From gravitons to gravity
74(5)
2.2.4 Effective field theories and the Planck scale
79(2)
2.3 Massive gravitons
81(14)
2.3.1 Phenomenological bounds
82(2)
2.3.2 Field theory of massive gravitons
84(11)
2.4 Solved problems
95(5)
2.1 The helicity of gravitons
95(3)
2.2 Angular momentum and parity of graviton states
98(2)
Further reading
100(1)
3 Generation of GWs in linearized theory
101(66)
3.1 Weak-field sources with arbitrary velocity
102(3)
3.2 Low-velocity expansion
105(4)
3.3 Mass quadrupole radiation
109(16)
3.3.1 Amplitude and angular distribution
109(4)
3.3.2 Radiated energy
113(1)
3.3.3 Radiated angular momentum
114(2)
3.3.4 Radiation reaction on non-relativistic sources
116(5)
3.3.5 Radiation from a closed system of point masses
121(4)
3.4 Mass octupole and current quadrupole
125(6)
3.5 Systematic multipole expansion
131(25)
3.5.1 Symmetric-trace-free (STF) form
134(5)
3.5.2 Spherical tensor form
139(17)
3.6 Solved problems
156(1)
3.1 Quadrupole radiation from an oscillating mass
156(2)
3.2 Quadrupole radiation from a mass in circular orbit
158(3)
3.3 Mass octupole and current quadrupole radiation from a mass in circular orbit
161(2)
3.4 Decomposition of Skl,m into irreducible representations of SO(3)
163(2)
3.5 Computation of integral dΩ(TE2B2lm)*ijni1...niα
165(1)
Further reading
166(1)
4 Applications
167(69)
4.1 Inspiral of compact binaries
167(33)
4.1.1 Circular orbits. The chirp amplitude
169(7)
4.1.2 Elliptic orbits. (I) Total power and frequency spectrum of the radiation emitted
176(8)
4.1.3 Elliptic orbits. (II) Evolution of the orbit under back-reaction
184(6)
4.1.4 Binaries at cosmological distances
190(10)
4.2 Radiation from rotating rigid bodies
200(15)
4.2.1 GWs from rotation around a principal axis
201(3)
4.2.2 GWs from freely precessing rigid bodies
204(11)
4.3 Radial infall into a black hole
215(9)
4.3.1 Radiation from an infalling point-like mass
215(4)
4.3.2 Tidal disruption of a real star falling into a black hole. Coherent and incoherent radiation
219(5)
4.4 Radiation from accelerated masses
224(6)
4.4.1 GWs produced in elastic collisions
224(3)
4.4.2 Lack of beaming of GWs from accelerated masses
227(3)
4.5 Solved problems
230(5)
4.1 Fourier transform of the chirp signal
230(3)
4.2 Fourier decomposition of elliptic Keplerian motion
233(2)
Further reading
235(1)
5 GW generation by post-Newtonian sources
236(66)
5.1 The post-Newtonian expansion
237(13)
5.1.1 Slowly moving, weakly self-gravitating sources
237(2)
5.1.2 PN expansion of Einstein equations
239(1)
5.1.3 Newtonian limit
240(2)
5.1.4 The 1PN order
242(3)
5.1.5 Motion of test particles in the PN metric
245(2)
5.1.6 Difficulties of the PN expansion
247(2)
5.1.7 The effect of back-reaction
249(1)
5.2 The relaxed Einstein equations
250(3)
5.3 The Blanchet-Damour approach
253(26)
5.3.1 Post-Minkowskian expansion outside the source
253(6)
5.3.2 PN expansion in the near region
259(4)
5.3.3 Matching of the solutions
263(3)
5.3.4 Radiative fields at infinity
266(9)
5.3.5 Radiation reaction
275(4)
5.4 The DIRE approach
279(3)
5.5 Strong-field sources and the effacement principle
282(7)
5.6 Radiation from inspiraling compact binaries
289(10)
5.6.1 The need for a very high-order computation
290(2)
5.6.2 The 3.5PN equations of motion
292(2)
5.6.3 Energy flux and orbital phase to 3.5PN order
294(2)
5.6.4 The waveform
296(3)
Further reading
299(3)
6 Experimental observation of GW emission in compact binaries
302(31)
6.1 The Hulse-Taylor binary pulsar
302(3)
6.2 The pulsar timing formula
305(21)
6.2.1 Pulsars as stable clocks
305(1)
6.2.2 Roemer, Shapiro and Einstein time delays
306(8)
6.2.3 Relativistic corrections for binary pulsars
314(12)
6.3 The double pulsar, and more compact binaries
326(5)
Further reading
331(2)
Part II: Gravitational-wave experiments
333(204)
7 Data analysis techniques
335(80)
7.1 The noise spectral density
335(4)
7.2 Pattern functions and angular sensitivity
339(4)
7.3 Matched filtering
343(3)
7.4 Probability and statistics
346(15)
7.4.1 Frequentist and Bayesian approaches
346(4)
7.4.2 Parameters estimation
350(6)
7.4.3 Matched filtering statistics
356(5)
7.5 Bursts
361(10)
7.5.1 Optimal signal-to-noise ratio
361(4)
7.5.2 Time-frequency analysis
365(4)
7.5.3 Coincidences
369(2)
7.6 Periodic sources
371(16)
7.6.1 Amplitude modulation
373(2)
7.6.2 Doppler shift and phase modulation
375(6)
7.6.3 Efficient search algorithms
381(6)
7.7 Coalescence of compact binaries
387(5)
7.7.1 Elimination of extrinsic variables
388(2)
7.7.2 The sight distance to coalescing binaries
390(2)
7.8 Stochastic backgrounds
392(21)
7.8.1 Characterization of stochastic backgrounds
393(4)
7.8.2 SNR for single detectors
397(3)
7.8.3 Two-detector correlation
400(13)
Further reading
413(2)
8 Resonant-mass detectors
415(55)
8.1 The interaction of GWs with an elastic body
415(12)
8.1.1 The response to bursts
415(5)
8.1.2 The response to periodic signals
420(1)
8.1.3 The absorption cross-section
421(6)
8.2 The read-out system: how to measure extremely small displacements
427(9)
8.2.1 The double oscillator
428(4)
8.2.2 Resonant transducers
432(4)
8.3 Noise sources
436(23)
8.3.1 Thermal noise
437(6)
8.3.2 Read-out noise and effective temperature
443(3)
8.3.3 Back-action noise and the quantum limit
446(3)
8.3.4 Quantum non-demolition measurements
449(4)
8.3.5 Experimental sensitivities
453(6)
8.4 Resonant spheres
459(10)
8.4.1 The interaction of a sphere with GWs
459(7)
8.4.2 Spheres as multi-mode detectors
466(3)
Further reading
469(1)
9 Interferometers
470
9.1 A simple Michelson interferometer
470(10)
9.1.1 The interaction with GWs in the TT gauge
471(5)
9.1.2 The interaction in the proper detector frame
476(4)
9.2 Interferometers with Fabry-Perot cavities
480(17)
9.2.1 Electromagnetic fields in a FP cavity
480(9)
9.2.2 Interaction of a FP cavity with GWs
489(5)
9.2.3 Angular sensitivity and pattern functions
494(3)
9.3 Toward a real GW interferometer
497(18)
9.3.1 Diffraction and Gaussian beams
497(7)
9.3.2 Detection at the dark fringe
504(6)
9.3.3 Basic optical layout
510(1)
9.3.4 Controls and locking
511(4)
9.4 Noise sources
515(13)
9.4.1 Shot noise
516(3)
9.4.2 Radiation pressure
519(3)
9.4.3 The standard quantum limit
522(2)
9.4.4 Displacement noise
524(4)
9.5 Existing and planned detectors
528(7)
9.5.1 Initial interferometers
528(4)
9.5.2 Advanced interferometers
532(3)
Further reading
535(2)
Bibliography
537(12)
Index
549
Gravitational Waves: Volume 2: Astrophysics and Cosmology
Part III: Astrophysical sources of gravitational waves
1(366)
10 Stellar collapse
3(71)
10.1 Historical Supernovae
4(6)
10.2 Properties of Supernovae
10(11)
10.2.1 SN classification
11(4)
10.2.2 Luminosities
15(3)
10.2.3 Rates
18(3)
10.3 The dynamics of core collapse
21(14)
10.3.1 Pre-SN evolution
21(4)
10.3.2 Core collapse and neutrino-driven delayed shock
25(5)
10.3.3 The remnant of the collapse
30(5)
10.4 GW production by self-gravitating fluids
35(11)
10.4.1 Energy-momentum tensor of a perfect fluid
35(3)
10.4.2 GW production from gravitating Newtonian fluids
38(4)
10.4.3 Quadrupole radiation from axisymmetric sources
42(4)
10.5 GWs from stellar collapse
46(20)
10.5.1 GWs from collapse and bounce of rotating cores
47(4)
10.5.2 GWs from bar-mode instabilities
51(4)
10.5.3 GWs from post-bounce convective instabilities
55(2)
10.5.4 GWs from anisotropic neutrino emission
57(5)
10.5.5 GWs from magneto-rotational core collapse
62(3)
10.5.6 GWs from fragmentation during collapse
65(1)
10.6 Complements: luminosity, color and metallicity of stars
66(5)
Further reading
71(3)
11 Neutron stars
74(41)
11.1 Observations of neutron stars
74(15)
11.1.1 The discovery of pulsars
74(1)
11.1.2 Pulsar spindown and the P-P plane
75(5)
11.1.3 Millisecond pulsars
80(1)
11.1.4 Pulsar demography
81(2)
11.1.5 SGRs and magnetars
83(6)
11.2 GW emission from neutron stars
89(22)
11.2.1 NS normal modes
89(10)
11.2.2 The CFS instability
99(7)
11.2.3 GWs from post-merger NS remnants
106(2)
11.2.4 GWs from deformed rotating NS
108(3)
Further reading
111(4)
12 Black-hole perturbation theory
115(74)
12.1 Scalar perturbations
115(2)
12.2 Gravitational perturbations
117(23)
12.2.1 Zerilli tensor harmonics
118(5)
12.2.2 The Regge-Wheeler gauge
123(4)
12.2.3 Axial perturbations: Regge-Wheeler equation
127(3)
12.2.4 Polar perturbations: Zerilli equation
130(1)
12.2.5 Boundary conditions
131(2)
12.2.6 The radiation field in the far zone
133(5)
12.2.7 Summary
138(2)
12.3 Black-hole quasi-normal modes
140(24)
12.3.1 General discussion
140(4)
12.3.2 QNMs from Laplace transform
144(7)
12.3.3 Power-law tails
151(6)
12.3.4 Frequency spectrum of QNMs
157(5)
12.3.5 The physical interpretation of the QNM spectrum
162(2)
12.4 Radial infall into a black hole
164(4)
12.4.1 The source term
165(1)
12.4.2 Numerical integration of the Zerilli equation
166(1)
12.4.3 Waveform and energy spectrum
167(1)
12.5 Perturbations of rotating black holes
168(12)
12.5.1 The Kerr metric
169(4)
12.5.2 Null tetrads and the Newman-Penrose formalism
173(4)
12.5.3 Teukolsky equation and QNMs of rotating BHs
177(3)
12.6 Solved problems
180(6)
12.1 Derivation of the Zerilli equation
180(4)
12.2 The source term for radial infall
184(2)
Further reading
186(3)
13 Properties of dynamical space-times
189(21)
13.1 The 3+1 decomposition of space-time
189(3)
13.2 Boundary terms in the gravitational action
192(3)
13.3 Hamiltonian formulation of GR
195(2)
13.4 Conserved quantities for isolated systems
197(10)
13.5 GWs and Newman-Penrose scalar
207(2)
Further reading
209(1)
14 GWs from compact binaries. Theory
210(67)
14.1 Non-perturbative resummations. A simple example
212(5)
14.2 Effective one-body action
217(24)
14.2.1 Equivalence to a one-body problem
217(10)
14.2.2 Conservative dynamics
227(3)
14.2.3 Inclusion of radiation reaction
230(1)
14.2.4 The EOB waveform
231(5)
14.2.5 Spinning binaries
236(5)
14.3 Numerical relativity
241(24)
14.3.1 Numerical integration of Einstein equations
241(3)
14.3.2 Equal-mass non-spinning BH binaries
244(4)
14.3.3 Unequal-mass non-spinning BH binaries
248(2)
14.3.4 Final BH recoil
250(3)
14.3.5 Spinning BHs and superkicks
253(7)
14.3.6 Astrophysical consequences of BH recoil
260(5)
14.4 GWs from NS-NS binaries
265(8)
14.4.1 Inspiral phase and tidal effects
265(5)
14.4.2 Merger phase and numerical relativity
270(3)
Further reading
273(4)
15 GWs from compact binaries. Observations
277(50)
15.1 GW150914. The first direct detection
278(12)
15.1.1 Evaluation of the statistical significance
279(6)
15.1.2 Properties of GW150914
285(5)
15.2 Further BH-BH detections
290(9)
15.2.1 GW151226
290(3)
15.2.2 GW170104
293(1)
15.2.3 GW170608
294(1)
15.2.4 GW170814: the first three-detector observation
295(2)
15.2.5 The population of BH-BH binaries
297(2)
15.3 GW170817: the first NS-NS binary
299(15)
15.3.1 GW observation
299(2)
15.3.2 The prompt-γ-ray burst
301(5)
15.3.3 The electromagnetic counterpart
306(3)
15.3.4 Kilonovae and r-process nucleosynthesis
309(2)
15.3.5 The cocoon scenario
311(3)
15.4 Tests of fundamental physics
314(8)
15.4.1 BH quasi-normal modes
314(2)
15.4.2 Tests of post-Newtonian gravity
316(1)
15.4.3 Propagation and degrees of freedom of GWs
317(5)
Further reading
322(5)
16 Supermassive black holes
327(40)
16.1 The central supermassive black hole in our Galaxy
327(3)
16.2 Supermassive black-hole binaries
330(9)
16.2.1 Formation and evolution of SMBH binaries
330(4)
16.2.2 SMBH binaries at LISA
334(5)
16.3 Extreme mass ratio inspirals
339(10)
16.3.1 Formation mechanisms
339(2)
16.3.2 EMRIs at LISA
341(2)
16.3.3 Waveforms and the self-force approach
343(6)
16.4 Stochastic GWs from SMBH binaries
349(14)
16.4.1 Regime dominated by GW back-reaction
351(1)
16.4.2 Regime dominated by three-body interactions
352(3)
16.4.3 High-frequency regime and source discreteness
355(2)
16.4.4 Estimates of the SMBH merger rate
357(2)
16.4.5 Effect of the eccentricity
359(4)
Further reading
363(4)
Part IV: Cosmology and gravitational waves
367(377)
17 Basics of FRW cosmology
369(43)
17.1 The FRW metric
369(5)
17.1.1 Comoving and physical coordinates
370(1)
17.1.2 Comoving and physical momenta
371(3)
17.2 Cosmological background equations for a single fluid
374(3)
17.3 Multi-component fluids
377(4)
17.4 RD-MD equilibrium, recombination and decoupling
381(2)
17.5 Effective number of relativistic species
383(5)
17.6 Conformal time and particle horizon
388(9)
17.6.1 Radiation dominance
389(2)
17.6.2 Matter dominance
391(1)
17.6.3 Analytic formulas in RD-EMD
392(1)
17.6.4 A dominance
393(1)
17.6.5 Conformal time at significant epochs
393(2)
17.6.6 Comoving distance, angular diameter distance and luminosity distance
395(2)
17.7 Newtonian cosmology inside the horizon
397(14)
17.7.1 Newtonian dynamics in expanding backgrounds
398(4)
17.7.2 Newtonian fluid dynamics in an expanding Universe
402(9)
Further reading
411(1)
18 Helicity decomposition of metric perturbations
412(25)
18.1 Perturbations around flat space
413(8)
18.1.1 Helicity decomposition
413(5)
18.1.2 Radiative and non-radiative degrees of freedom
418(3)
18.2 Gauge invariance and helicity decomposition in FRW
421(4)
18.2.1 Linearized diffeomorphisms and gauge invariance in a curved background
421(1)
18.2.2 Bardeen variables
422(3)
18.3 Perturbed energy-momentum tensor
425(11)
18.3.1 General decomposition of Tμν
426(2)
18.3.2 Perturbations of perfect fluids
428(3)
18.3.3 Linearized energy-momentum conservation
431(3)
18.3.4 Gauge-invariant combinations
434(2)
Further reading
436(1)
19 Evolution of cosmological perturbations
437(70)
19.1 Evolution equations in the scalar sector
437(10)
19.1.1 Single-component fluid
439(2)
19.1.2 Multi-component fluid
441(2)
19.1.3 Super-horizon and sub-horizon regimes
443(4)
19.2 Initial conditions
447(7)
19.2.1 Adiabatic and isocurvature perturbations
449(2)
19.2.2 The variables ζ and R
451(3)
19.3 Solutions of the equations for scalar perturbations
454(10)
19.3.1 Numerical integration
454(4)
19.3.2 Analytic solutions in RD
458(3)
19.3.3 Analytic solutions in MD
461(2)
19.3.4 Analytic solutions during dark-energy dominance
463(1)
19.4 Power spectra for scalar perturbations
464(10)
19.4.1 Definitions and conventions
464(2)
19.4.2 The primordial power spectrum
466(3)
19.4.3 Transfer function and growth rate
469(3)
19.4.4 The linearly processed power spectrum
472(2)
19.5 Tensor perturbations
474(18)
19.5.1 Cosmological evolution
474(8)
19.5.2 Transfer function for tensor modes
482(4)
19.5.3 GW damping from neutrino free-streaming
486(2)
19.5.4 The tensor power spectrum, &Qmega;gw(f) and hc(f)
488(4)
19.6 Standard sirens, dark energy and modified gravity
492(13)
19.6.1 Testing cosmological models against observations
494(2)
19.6.2 Cosmology with standard sirens
496(4)
19.6.3 Tensor perturbations in modified gravity
500(2)
19.6.4 An explicit example: non-local gravity
502(3)
Further reading
505(2)
20 The imprint of GWs on the CMB
507(67)
20.1 The CMB multipoles
507(5)
20.2 Null geodesics
512(5)
20.3 Temperature anisotropies at large angles
517(28)
20.3.1 Photon geodesics in a perturbed FRW metric
517(2)
20.3.2 Sachs-Wolfe, ISW and Doppler contributions
519(4)
20.3.3 Expression of the Cl in terms of the Θl(k)
523(3)
20.3.4 Scalar contribution to the Cl
526(4)
20.3.5 Tensor contribution to the Cl
530(8)
20.3.6 Finite thickness of the LSS
538(2)
20.3.7 The Boltzmann equation for photons
540(5)
20.4 CMB polarization
545(26)
20.4.1 Stokes parameters
545(3)
20.4.2 Polarization maps. E and B modes
548(3)
20.4.3 Polarization and tensor spherical harmonics
551(7)
20.4.4 Generation of CMB polarization
558(11)
20.4.5 Experimental situation
569(2)
Further reading
571(3)
21 Inflation and primordial perturbations
574(70)
21.1 Inflationary cosmology
574(21)
21.1.1 The flatness problem
574(4)
21.1.2 The horizon problem
578(2)
21.1.3 Single-field slow-roll inflation
580(4)
21.1.4 Large-field and small-field inflation
584(6)
21.1.5 Starobinsky model
590(5)
21.2 Quantum fields in curved space
595(15)
21.2.1 Field quantization in curved space
595(6)
21.2.2 Quantum fields in a FRW background
601(2)
21.2.3 Vacuum fluctuations in de Sitter inflation
603(7)
21.3 Primordial perturbations in single-field slow-roll inflation
610(31)
21.3.1 Mukhanov-Sasaki equation
611(2)
21.3.2 Scalar perturbations to lowest order in slowroll
613(1)
21.3.3 Scalar perturbations to first order. Spectral tilt
614(6)
21.3.4 Tensor perturbations
620(4)
21.3.5 Predictions from a sample of inflationary models
624(5)
21.3.6 The relic inflationary GW background today
629(7)
21.3.7 A full quantum computation of Ωgw(f)
636(5)
Further reading
641(3)
22 Stochastic backgrounds of cosmological origin
644(79)
22.1 Characteristic frequency of relic GWs
644(3)
22.2 GW production by classical fields
647(6)
22.2.1 General formalism
647(4)
22.2.2 GW generation by a stochastic scalar field
651(2)
22.3 GWs from preheating after inflation
653(4)
22.3.1 Parametric resonance in single-field inflation
653(3)
22.3.2 Tachyonic preheating in hybrid inflation
656(1)
22.4 GWs from first-order phase transitions
657(27)
22.4.1 Crossovers and phase transitions
657(4)
22.4.2 First-order phase transitions in cosmology
661(2)
22.4.3 Thermal tunneling theory
663(12)
22.4.4 Bubble dynamics and GW production
675(9)
22.5 Cosmic strings
684(21)
22.5.1 Global and local strings
684(4)
22.5.2 Effective description and Nambu-Goto action
688(4)
22.5.3 String dynamics. Cusps and kinks
692(5)
22.5.4 Gravitational radiation from cosmic strings
697(8)
22.6 Alternatives to inflation
705(5)
22.7 Bounds on primordial GW backgrounds
710(10)
22.7.1 The nucleosynthesis bound
710(7)
22.7.2 Bounds on extra radiation from the CMB
717(1)
22.7.3 Bounds from the CMB at large angles
718(1)
22.7.4 Limits on stochastic backgrounds from interferometers
719(1)
Further reading
720(3)
23 Stochastic backgrounds and pulsar timing arrays
723(21)
23.1 GW effect on the timing of a single pulsar
724(5)
23.2 Response to a continuous signal
729(1)
23.3 Response to a stochastic GW background
730(4)
23.4 Extracting the GW signal from noise
734(7)
23.5 Searches for stochastic backgrounds with PTAs
741(1)
Further reading
742(2)
Bibliography
744(71)
Index
815
Michele Maggiore is Professor of Physics at the Department of Theoretical Physics, University of Geneva, Switzerland. He served as President of the Physics Section at the University of Geneva until 2017.