Contents

Preface	xiii
1 The Cosmological Parameters	1
1.1 Introduction	1
1.2 Why Measure the Parameters?	2
1.2.1 Testing the Physics	2
1.2.2 How Will It All End?	7
1.3 The State of the Measurements	11
1.4 Cosmology for the Next Generation	17
2 In the Beginning...	25
2.1 The Future Fate of Cosmology	25
2.2 Testing Inflation	27
2.3 The Power of the Cosmic Microwave Background	28
2.4 Cosmic Concordance	35
2.5 A New Age?	40
3 Understanding Data Better with Bayesian and Global Statistical Methods	49
3.1 Introduction	49
3.2 Combining Experimental Measurements	50
3.3 Bayesian Combination of Incompatible Measurements	51
3.4 Another Variant of the Method	56
3.5 Results for the Hubble Constant	56
3.6 Conclusion	59
4 Large-Scale Structure in the Universe	61
4.1 Introduction	61
4.2 Clustering and Large-Scale Structure	65
4.2.1 Galaxies and Large-Scale Structure	65
4.2.2 Clusters and Large-Scale Structure	69
4.3 Peculiar Motions on Large Scales	74
4.4 Dark Matter and Baryons in Clusters of Galaxies	79
4.5 Is < 1?	81
4.6 The SDSS and Large-Scale Structure	82
4.6.1 The Sloan Digital Sky Survey	82
4.6.2 Clusters of Galaxies	83
4.7 Summary	86
5 Unsolved Problems in Gravitational Lensing	93
5.1 Introduction	94
5.2 Gravitational Lens Optics	94
5.3 The Problems	98
5.3.1 How Old Is the Universe?	98
5.3.2 What Is the Shape of the Universe?	101
5.3.3 What Is the Large Scale Distribution of Matter?	101
5.3.4 How Are Rich Clusters of Galaxies Formed?	102
5.3.5 When Did Galaxies Form and How Did They Evolve?	105
5.3.6 How Big Are Galaxies?	106
5.3.7 Of What Are Galaxies Made?	107
5.3.8 How Big Are AGN Ultraviolet Emission Regions?	107
5.4 How Many More Surprises Will Gravitational Lenses Provide?	108
6 What Can Be Learned from Numerical Simulations of Cosmology	115
6.1 Introduction	116
6.2 Simulation Methods	119
6.2.1 Specification of Models	119
6.2.2 Physical Processes and Numerical Methods	122
6.3 Results: Comparison with Observations	126
6.3.1 Hot Components	126
6.3.2 Warm Components	127
6.3.3 Cold Condensed Components	128
6.4 Conclusions, Prospects, and More Questions	129
7 The Centers of Elliptical Galaxies	137
7.1 Introduction	137
7.1.1 Black Holes and Quasars	138
7.1.2 The Sphere of Influence	139
7.1.3 Cores and Cusps	140
7.2 Photometry	142
7.2.1 The Peebles-Young Model	145
7.3 Kinematic Evidence for Central Black Holes	147
7.4 Physical Processes	148
7.5 Summary	152
8 The Morphological Evolution of Galaxies	159
8.1 Introduction	159
8.2 Early Formation of Massive Ellipticals	161
8.3 Slow Evolution of Massive Disk Galaxies	164
8.4 Redshift Surveys and the Dwarf-Dominated Universe	166
8.5 Faint Galaxy Morphologies from HST	170
8.6 Conclusions	174
9 Quasars	181
9.1 Quasars and the End of the `Dark Age'	181
9.2 The Relation of AGNs to the Central Bulges of Galaxies	183
9.3 Quasars and Their Remnants: Probes of General Relativity?	186
9.3.1 Dead Quasars in Nearby Galaxies	186
9.3.2 Do These Holes Have a Kerr Metric?	187
10 Solar Neutrinos: Solved and Unsolved Problems	195
10.1 Why Study Solar Neutrinos?	195
10.2 What Does the Combined Standard Model Tell Us About Solar Neutrinos?	198
10.2.1 The Combined Standard Model	198
10.2.2 The Solar Neutrino Spectrum	200
10.3 Why Are the Predicted Neutrino Fluxes Robust?	201
10.4 What Are the Three Solar Neutrino Problems?	202
10.4.1 Calculated versus Observed Chlorine Rate	203
10.4.2 Incompatibility of Chlorine and Water (Kamiokande) Experiments	204
10.4.3 Gallium Experiments: No Room for 7Be Neutrinos	205
10.5 What Have We Learned?	206
10.5.1 About Astronomy	206
10.5.2 About Physics	208
10.6 What Next?	209
10.6.1 Solvable Problems in Physics	209
10.6.2 Solvable Problems in Astronomy	212
10.7 Summary	217
11 Particle Dark Matter	221
11.1 Introduction: Three Arguments for Non-Baryonic Dark Matter	221
11.2 The Case for Non-baryonic Matter	222
11.2.1 We've Looked for Baryonic Dark Matter and Failed	222
11.2.2 We Can't Seem To Make the Observed Large-Scale Structure with Baryons	223
11.2.3 Dynamical Mass Is Much Larger than Big Bang Nucleosynthesis Allows	224
11.3 Neutrinos As Dark Matter	225
11.3.1 Detecting Massive Neutrinos	226
11.4 WIMPs	227
11.4.1 Searching for WIMPs	228
11.4.2 Indirect WIMP Detection	230
11.4.3 What Is To Be Done?	231
11.5 Axions	231
11.6 Conclusions	233
12 Stars in the Milky Way and Other Galaxies	241
12.1 Introduction	241
12.2 Recent Star Count Results	241
12.3 Microlensing and Star Counts	243
12.4 Disk Dark Matter: Still a Question	243
12.5 Mystery of the Long Events	244
12.6 Proper Motions from EROS II	245
12.7 Pixel Lensing: Stellar Mass Functions in Other Galaxies	246
12.8 Star Formation History of the Universe	248
12.9 Conclusions	249
13 Searching for MACHOs with Microlensing	253
13.1 Introduction	253
13.2 The Gravitational Microlens	254
13.3 The "Macho Fraction" in the Galactic Halo	256
13.4 The Experimental Situation	258
13.5 Next Generation Experiments	260
13.5.1 What Can Be Achieved from the Ground?	260
13.5.2 Observing Macho Parallax	261
13.6 Working on Gravitational Microlensing	263
13.7 Summary	264
13.7.1 What We Know Now	264
13.7.2 What We Will Learn from Current Experiments	264
13.7.3 Next Generation Experiments	264
13.8 Late Breaking News	265
14 Globally Asymmetric Supernova	269
14.1 Introduction	269
14.1.1 Preamble	269
14.1.2 Evidence for Asymmetry	270
14.1.3 State of the Art	271
14.2 Instability During Core Collapse	272
14.2.1 Accomplishments	273
14.2.2 Future Directions	273
14.3 Overstable Core g-Modes	274
14.3.1 Accomplishments	275
14.3.2 Future Directions	276
14.3.3 Turbulent Excitation of g-Modes	277
15 In and around Neutron Stars	281
15.1 Introduction	281
15.2 Superfluid-Superconductor Interactions in a Neutron Star Core	284
15.3 The Stellar Crust	288
15.4 Spun-up Neutron Stars	289
15.5 Spinning-down Radiopulsars	293
15.6 Glitches of Radiopulsar Spin Periods	294
16 Accretion Flows around Black Holes	301
16.1 Introduction	301
16.2 X-rays and -rays from Accreting Black Holes	302
16.3 Hot Accretion Flow Models	304
16.3.1 Corona Models	305
16.3.2 SLE Two-Temperature Model	306
16.3.3 Optically-Thin Advection-Dominated Model	306
16.4 Directions for Future Research	311
16.4.1 Unresolved Theoretical Issues	311
16.4.2 Clues from Observations of Black Hole XRBs	313
16.4.3 Black Holes versus Neutron Stars	315
16.5 Conclusion	316
17 The Highest Energy Cosmic Rays	325
17.1 Introduction	325
17.2 Review of Existing Data on the Highest Energy Cosmic Rays	327
17.3 Acceleration and Transport of the Cosmic Rays   1019 eV	329
17.4 The Big Events	332
17.5 The Auger Project	335
17.6 What Can We Learn from Two Large Surface Arrays?	337
17.7 Should a Student Work on This Problem?	338
17.8 Final Remark	339
18 Toward Understanding Gamma-Ray Bursts	343
18.1 Introduction	343
18.2 Observations	344
18.2.1 Observational Open Questions	348
18.3 A Brief Summary	348
18.4 Where?	349
18.5 How?	349
18.5.1 The Compactness Problem	350
18.5.2 Relativistic Motion	351
18.5.3 Slowing Down of Relativistic Particles	354
18.5.4 The Acceleration Mechanism?	362
18.6 What?	364
18.6.1 What Do We Need from the Internal Engine?	364
18.6.2 Coincidences and Other Astronomical Hints	365
18.7 Why?	367
18.8 Conclusions	369
18.9 Some Open Questions	369