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Gravitational-Wave Astronomy: Exploring the Dark Side of the Universe [Kõva köide]

(Professor of Applied Mathematics, University of Southampton)
  • Formaat: Hardback, 688 pages, kõrgus x laius x paksus: 252x175x38 mm, kaal: 1444 g, 116 color and 51 grayscale line figures; 1 color halftone
  • Sari: Oxford Graduate Texts
  • Ilmumisaeg: 28-Nov-2019
  • Kirjastus: Oxford University Press
  • ISBN-10: 0198568037
  • ISBN-13: 9780198568032
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  • Formaat: Hardback, 688 pages, kõrgus x laius x paksus: 252x175x38 mm, kaal: 1444 g, 116 color and 51 grayscale line figures; 1 color halftone
  • Sari: Oxford Graduate Texts
  • Ilmumisaeg: 28-Nov-2019
  • Kirjastus: Oxford University Press
  • ISBN-10: 0198568037
  • ISBN-13: 9780198568032
Teised raamatud teemal:
This book is an introduction to gravitational waves and related astrophysics. It provides a bridge across the range of astronomy, physics and cosmology that comes into play when trying to understand the gravitational-wave sky. Starting with Einstein's theory of gravity, chapters develop the key ideas step by step, leading up to the technology that finally caught these faint whispers from the distant universe. The second part of the book makes a direct connection with current research, introducing the relevant language and making the involved concepts less mysterious. The book is intended to work as a platform, low enough that anyone with an elementary understanding of gravitational waves can scramble onto it, but at the same time high enough to connect readers with active research - and the many exciting discoveries that are happening right now.

The first part of the book introduces the key ideas, following a general overview chapter and including a brief reminder of Einstein's theory. This part can be taught as a self-contained one semester course. The second part of the book is written to work as a collection of "set pieces" with core material that can be adapted to specific lectures and additional material that provide context and depth.

A range of readers may find this book useful, including graduate students, astronomers looking for basic understanding of the gravitational-wave window to the universe, researchers analysing data from gravitational-wave detectors, and nuclear and particle physicists.
1 Opening the window
1(94)
1.1 The beginning
1(2)
1.2 A new kind of astronomy
3(3)
1.3 Audio not video
6(1)
1.4 On the back of an envelope
7(3)
1.5 Binary inspiral and merger
10(4)
1.6 Supernovae
14(1)
1.7 Spinning neutron stars
15(3)
1.8 Fundamental physics
18(1)
1.9 Many different messengers
18(1)
1.10 The golden binary
19(6)
Part 1 From theory to experiment
2 A brief survey of general relativity
25(2)
2.1 A simple thought experiment
27(1)
2.2 The tidal tensor
28(3)
2.3 Introducing the metric
31(3)
2.4 The four-velocity
34(5)
2.5 The covariant derivative
39(2)
2.6 The geodesic equation
41(2)
2.7 Curvature
43(2)
2.8 A little bit of matter
45(2)
2.9 Geodesic deviation and Einstein's equations
47(4)
3 Gravitational waves
51(22)
3.1 Weak waves in an otherwise flat spacetime
52(2)
3.2 Effect on matter
54(2)
3.3 The wave equation
56(2)
3.4 Transverse-traceless (TT) gauge
58(3)
3.5 The quadrupole formula
61(3)
3.6 The energy carried by gravitational waves
64(3)
3.7 The radiation reaction force
67(3)
3.8 The radiated angular momentum
70(1)
3.9 A stab at perturbation theory
71(2)
4 From black holes to stars and the Universe at large
73(17)
4.1 The Schwarzschild solution
73(2)
4.2 Relativistic fluids
75(2)
4.3 How to build a star
77(1)
4.4 The Newtonian limit
78(4)
4.5 Modelling the Universe
82(3)
4.6 Was Einstein right?
85(5)
5 Binary inspiral
90(15)
5.1 Basic celestial mechanics
90(5)
5.2 Circular orbits
95(3)
5.3 The Binary Pulsar
98(1)
5.4 Eccentic orbits
99(3)
5.5 The orbital evolution
102(3)
6 Spinning stars and cosmic recycling
105(20)
6.1 Rotating deformed stars
105(5)
6.2 The Crab Pulsar
110(2)
6.3 Contact binaries
112(4)
6.4 Cosmic recycling
116(3)
6.5 Spin-orbit evolution
119(6)
7 Catching the wave
125(25)
7.1 Resonant mass detectors
126(2)
7.2 Gravitational waves and light beams
128(5)
7.3 Advanced interferometers
133(4)
7.4 An international network
137(3)
7.5 The antenna pattern
140(2)
7.6 The road to the future
142(6)
7.7 Doppler tracking
148(1)
7.8 Pulsar timing arrays
149(1)
8 Mining the data
150(27)
8.1 Random noise
151(2)
8.2 Matched filtering and the optimal signal-to-noise ratio
153(4)
8.3 Applications of matched filtering
157(4)
8.4 Bursts searches
161(2)
8.5 Stochastic backgrounds
163(2)
8.6 Avoiding false alarms
165(2)
8.7 Bayesian inference
167(4)
8.8 Geometry in signal analysis
171(6)
Part 2 The dark side of the universe
9 The stellar graveyard
177(30)
9.1 White dwarfs
178(2)
9.2 The Fermi gas model
180(2)
9.3 Chandrasekhar's limit
182(2)
9.4 Neutron stars
184(5)
9.5 The rebirth of relativity
189(2)
9.6 Weighing black holes
191(4)
9.7 The formation of compact binaries
195(4)
9.8 Estimating merger rates
199(3)
9.9 Active galaxies
202(2)
9.10 A giant at the centre of the Milky Way
204(3)
10 Testing relativity
207(22)
10.1 Geodesies
208(2)
10.2 The gravitational redshift
210(1)
10.3 Flying clocks
211(2)
10.4 Light bending
213(2)
10.5 Shapiro time delay
215(1)
10.6 Light rays and black holes
216(2)
10.7 The motion of massive bodies
218(2)
10.8 Perihelion precession
220(1)
10.9 The Double pulsar
221(2)
10.10 Radial infall
223(2)
10.11 A bit more celestial mechanics
225(4)
11 Beyond Newton
229(21)
11.1 Near and far-zone solutions
230(5)
11.2 A slight aside: symmetric trace-free (STF) tensors
235(2)
11.3 The relaxed Einstein equations
237(3)
11.4 Iterative schemes
240(2)
11.5 Inspiralling binaries
242(5)
11.6 The effective one body approach
247(3)
12 Towards the extreme
250(32)
12.1 Matter at supranuclear densities
250(2)
12.2 A simple model for npe matter
252(2)
12.3 Determining the equation of state
254(5)
12.4 Observational constraints
259(1)
12.5 The slow-rotation approximation
260(2)
12.6 The virial theorem
262(4)
12.7 The Kepler limit
266(2)
12.8 Rotating relativistic stars
268(4)
12.9 The quasiradial instability
272(2)
12.10 Superfluids and glitches
274(8)
13 From oscillations to instabilities
282(30)
13.1 The fundamental f-mode
282(5)
13.2 General non-rotating stars: p/g-modes
287(5)
13.3 Calculating stellar oscillation modes
292(3)
13.4 The r-modes
295(3)
13.5 Gravitational-wave emission
298(1)
13.6 What do we learn from the ellipsoids?
299(6)
13.7 Lagrangian perturbation theory for rotating stars
305(4)
13.8 The CFS instability
309(3)
14 Building mountains
312(49)
14.1 The crust
312(4)
14.2 Energetics
316(4)
14.3 Modelling elastic deformations
320(7)
14.4 Searches for known pulsars
327(2)
14.5 All-sky searches
329(4)
14.6 The magnetic field
333(4)
14.7 The birth of a magnetar
337(2)
14.8 Modelling accretion
339(5)
14.9 The low-mass X-ray binaries
344(4)
14.10 Magnetic field burial and confinement
348(3)
14.11 Persistent sources
351(2)
14.12 Free precession
353(4)
14.13 Evolution of the wobble angle
357(4)
15 The r-mode instability
361(30)
15.1 The instability window
362(5)
15.2 Complicating factors
367(5)
15.3 A simple spin-evolution model
372(5)
15.4 Nonlinear saturation
377(4)
15.5 Are the gravitational waves detectable?
381(2)
15.6 Astrophysical constraints for young neutron stars
383(4)
15.7 r-modes in accreting systems
387(4)
16 Black-hole dynamics
391(28)
16.1 Issues of stability
391(1)
16.2 Scalar field dynamics
392(7)
16.3 Gravitational perturbations
399(6)
16.4 Quasinormal modes
405(2)
16.5 Test particle motion
407(3)
16.6 Taking the plunge
410(9)
16.7 The self-force problem
419(1)
17 Spinning black holes
419(24)
17.1 The Kerr solution
419(1)
17.2 Inertial framedragging
419(2)
17.3 Kerr geodesies
421(3)
17.4 The Newman-Penrose formalism
424(10)
17.5 The Teukolsky equation
434(5)
17.6 Kerr quasinormal modes
439(1)
17.7 GW150914: A faint fingerprint
440(3)
18 Relativistic asteroseismology
443(36)
18.1 Relativistic fluid perturbations
443(4)
18.2 f-and p-modes in relativity
447(5)
18.3 The inverse problem
452(2)
18.4 The w-modes
454(3)
18.5 The evolving spectrum of adolescent neutron stars
457(5)
18.6 Magnetar seismology
462(3)
18.7 The relativistic r-modes
465(5)
18.8 The unstable f-modes
470(9)
19 Colliding black holes
479(29)
19.1 The 3+1 decomposition
482(2)
19.2 Evolving the spacetime
484(2)
19.3 Initial data
486(3)
19.4 Slicing conditions
489(2)
19.5 Wave extraction
491(2)
19.6 2 + 2 and the Bondi news
493(3)
19.7 Milestones and breakthroughs
496(6)
19.8 Recoil and kicks
502(6)
20 Cosmic fireworks
508(33)
20.1 Simulating fluids
508(5)
20.2 The bar-mode instability
513(3)
20.3 Tidal disruption
516(3)
20.4 Black hole--neutron star mergers
519(3)
20.5 Magnetohydrodynamics
522(3)
20.6 The magnetorotational instability
525(3)
20.7 Gravitational collapse
528(3)
20.8 Supernova core collapse
531(8)
20.9 Hypernovae
539(2)
21 Anatomy of a merger
541(40)
21.1 GW170817
541(2)
21.2 Tidal deformation
543(8)
21.3 The relativistic Love number
551(5)
21.4 Dynamical tides: resonances
556(7)
21.5 Shattering the crust
563(2)
21.6 Merger dynamics
565(7)
21.7 Gamma-ray bursts
572(6)
21.8 The signature of a kilonova
578(3)
22 Whispers from the Big Bang
581(2)
22.1 The standard model of cosmology
583(4)
22.2 The cosmological redshift
587(2)
22.3 Scaling the distance ladder
589(2)
22.4 Standard sirens
591(3)
22.5 Geometrical optics and lensing
594(4)
22.6 Astrophysical backgrounds
598(4)
22.7 Pulsar timing arrays
602(7)
22.8 AC/DC
609(1)
22.9 Astrometry
609(2)
22.10 Detecting a primordial background
611(2)
22.11 Parametric amplification of quantum fluctuations
613(3)
22.12 Phase transitions
616(1)
22.13 Cosmic strings
617(2)
22.14 E/B-modes
619(1)
22.15 Twenty-nine decades of frequency
620(5)
Apologies and thanks 625(2)
References 627(34)
Index 661
Nils Andersson is a professor of mathematics and an expert on Einstein's theory of relativity and related astrophysics. His research mainly concerns black holes, neutron stars and gravitational waves. Over the last couple of decades, he has actively pursued many issues relevant to the emerging area of gravitational-wave astronomy. His current work focuses on the extreme physics that neutron stars represent, from the state and composition of matter to the dynamical role of the superfluid and superconducting components expected to be present in the core of a mature neutron star.