Aschenbach / Burwitz / Hasinger Relativistic Astrophysics and Cosmology - Einstein's Legacy

Proceedings of the MPE/USM/MPA/ESO Joint Astronomy Conference Held in Munich, Germany, 7-11 November 2005
2007
ISBN: 978-3-540-74713-0
Verlag: Springer Berlin Heidelberg
Format: PDF
Kopierschutz: 1 - PDF Watermark

E-Book, Englisch, 506 Seiten

Reihe: ESO Astrophysics Symposia

The year 2005, which marked the 100th anniversary of the 'annus mirabilis', the year in which Albert Einstein published three of his most important scientific papers, was the perfect opportunity to review and to present the current scientific understanding of relativistic topics. This book provides an up-to-date reference on the theory of gravity, relativistic astrophysics and cosmology. It is a useful reference tool for both the expert and the new-comer in these fields.

Autoren/Hrsg.

Aschenbach, Bernd

Burwitz, Vadim

Hasinger, Günther

Leibundgut, Bruno

Inhaltsverzeichnis

1;Preface;5
2;Contents;8
3;List of Participants;17
4;Scientific Advisory Comittee;30
5;Local Organizing Comittee;30
6;Invited Speakers;30
7;Cosmology;32
7.1;Structure Formation in a Variable Dark Energy Model and Observational Constraints;33
7.1.1;1 Introduction;33
7.1.2;2 Structure Formation in the Variable Dark Energy Model;34
7.1.3;3 Observational Constraints on the Dark Energy Model;35
7.1.4;4 Conclusions;37
7.1.5;References;37
7.2;Effect of the Rotation of the Universe on the Energy Levels of Hydrogen Atoms;38
7.2.1;1 Shell Model and Spin-Spin Interaction;38
7.2.2;2 G AE odel Universe and Lamb Shift of Hydrogen;39
7.2.3;3 Discussion;40
7.2.4;References;40
7.3;Modified Chaplygin Gas and Accelerated Universe;41
7.3.1;1 Introduction;41
7.3.2;2 Modified Chaplygin Gas in FRWModel;42
7.3.3;3 The Role of StateFinder Parameters in FRW Universe;43
7.3.4;4 Discussions;45
7.3.5;References;45
7.4;Spherically Symmetric, Static Spacetimes in a Tensor- Vector- Scalar Theory;46
7.4.1;1 Introduction;46
7.4.2;2 The Basic Equations of TeVeS;47
7.4.3;3 Spherical Symmetric, Static Spacetimes;47
7.4.4;4 Analytic Solution when Ur Vanishes;49
7.4.5;5 Conclusions;50
7.4.6;References;50
7.5;Type Ia Supernovae and Cosmology;51
7.5.1;1 Introduction;51
7.5.2;2 Modeling type Ia supernovae;52
7.5.3;3 Some simulation results;53
7.5.4;4 Predictions for observable quantities;54
7.5.5;5 Summary and conclusions;56
7.5.6;References;57
7.6;Path and Path Deviation Equations in Kaluza-Klein Type Theories: A Brief Introduction*;59
7.6.1;1 The Bazanski Approach in 5D;59
7.6.2;2 Rotation in 5D;60
7.6.3;References;61
7.7;Studying Dark Energy with Galaxy Clusters;62
7.7.1;1 Introduction;62
7.7.2;2 Self Calibration in Cluster Surveys;63
7.7.3;3 Dark Energy Constraints from Upcoming Surveys: An Example;65
7.7.4;4 Final Comments;67
7.7.5;References;67
7.8;Astrophysical Tests of Fundamental Physics;68
7.8.1;References;72
7.9;Slow-roll Corrections to Inflation Fluctuations on a Brane;73
7.9.1;1 Introduction and Motivation;73
7.9.2;2 Summary and Discussions;74
7.9.3;References;75
7.10;Statistical Mechanics of the SDSS Galaxy Distribution;76
7.10.1;1 Introduction;76
7.10.2;2 Theoretical Models;76
7.10.3;3 Comparison with Observation;77
7.10.4;References;79
7.11;The Second-Order Cosmological Perturbation and the Large Scale Structure Formation;80
7.11.1;1 Introduction;80
7.11.2;2 Equations;81
7.11.3;3 Correspondence;81
7.11.4;4 Summary;82
7.12;Supermassive Black Holes in Galaxies;83
7.12.1;1 Introduction;83
7.12.2;2 Analysis of the NGC 4486a Data;84
7.12.3;3 Outlook;85
7.12.4;References;85
7.13;Lagrangian Description for the Cosmic Fluid;86
7.13.1;1 Linear Perturbation;86
7.13.2;2 Higher-Order Approximation;86
7.13.3;3 The Validity of Lagrangian Description;87
7.13.4;4 Future Prospect;87
7.13.5;References;88
7.14;MachÌs Principle and a Variable Speed of Light;89
7.14.1;1 Riddles in Gravitational Physics;89
7.14.2;2 MachÌs Principle;90
7.14.3;3 SciamaÌs Version of MachÌs Principle.;90
7.14.4;4 Einstein and a Variable c.;90
7.14.5;5 The Equivalence Principle;91
7.14.6;6 c as a Function of the Mass Distribution in the Universe;91
7.14.7;7 Visible Matter and Flatness;92
7.14.8;8 Outlook;92
7.14.9;References;93
7.15;A Century of Cosmology;94
7.15.1;1 Introduction;94
7.15.2;2 Einstein and .;94
7.15.3;3 Big Bang vs. Steady State;95
7.15.4;4 Discovery and Non-discovery of the CMB;96
7.15.5;5 Nucleosynthesis;97
7.15.6;6 CMB Anisotropy;97
7.15.7;7 Supernovae;99
7.15.8;8 Search for Two Numbers;99
7.15.9;9 Discussion;101
7.15.10;References;101
8;Gravity;103
8.1;The Stochastic Gravitational-Wave Background from Cold Dark Matter Halos;104
8.1.1;1 The Hybrid Approximation and the Most-Probable Halo;104
8.1.2;2 Results and Conclusions;105
8.1.3;References;106
8.2;GravitationalWave from Realistic Stellar Collapse : Odd Parity Perturbation;108
8.2.1;1 Introduction;108
8.2.2;2 Set Up and Numerical Result;108
8.2.3;3 Conclusion;110
8.2.4;References;110
8.3;Finding the Electromagnetic Counterparts of Standard Sirens;111
8.3.1;1 Introduction;111
8.3.2;2 The GW Error Volume;112
8.3.3;3 Search for Quasar Counterparts;113
8.3.4;4 Conclusions;114
8.3.5;References;115
8.4;Strong-Field Tests of Gravity with the Double Pulsar;116
8.4.1;1 Introduction;116
8.4.2;2 Strong-Field Tests with the Double Pulsar;117
8.4.3;3 Further and Future Measurements;119
8.4.4;4 Summary & conclusions;119
8.4.5;References;119
8.5;The Relativistic Time Delay of the Pulsar Radiation in the Non- Stationary Gravitational Field of the Globular Clusters;121
8.5.1;References;123
8.6;Relativistic Bose-Einstein Condensation Model for Dark Matter and Dark Energy;124
8.6.1;1 Introduction;124
8.6.2;2 BEC in the Universe;125
8.6.3;3 Observational Constraints;126
8.6.4;4 Conclusions;126
8.6.5;References;126
8.7;Equilibrium Configurations of Degenerate Fermionic Dark Matter and the Black Hole Mass Hierarchy;127
8.7.1;1 Introduction;127
8.7.2;2 Structures Formed by Degenerate Fermions;127
8.7.3;3 Flat-top Structures at the Centre of A1689 Ò Hybrid State Equation Ò;128
8.7.4;References;129
8.8;Hardening in a Stellar Time-Evolving Background: Prospects for LISA;130
8.8.1;1 Introduction;130
8.8.2;2 Star-Binary Interactions;131
8.8.3;3 Conclusions;133
8.8.4;References;134
8.9;GravitationalWaves for Odd Parity from a Collapsing Dust Ball;135
8.9.1;1 Introduction;135
8.9.2;2 Basic Equations;135
8.9.3;3 Conclusion and Discussion;137
8.9.4;References;137
9;Black Holes;138
9.1;The Supermassive Black-Hole Mass Estimation in the Sy1.9 Galaxy SBS 0748+ 499;139
9.1.1;1 Introduction;139
9.1.2;2 Discussion;141
9.1.3;References;141
9.2;Accretion of StellarWinds in the Galactic Centre;143
9.2.1;1 Introduction;143
9.2.2;2 Method and Initial Conditions;144
9.2.3;3 Results;144
9.2.4;4 Conclusions;146
9.2.5;References;147
9.3;Winds Driven by Line Opacity near Neutron Stars and Black Holes;148
9.3.1;1 Introduction;148
9.3.2;2 Gravitationally Exposed Flow;150
9.3.3;3 Discussion;150
9.3.4;References;151
9.4;Inspiral of Double Black Holes in Gaseous Nuclear Disks;153
9.4.1;1 Introduction;153
9.4.2;2 The Simulations;154
9.4.3;3 Conclusion;155
9.4.4;References;155
9.5;The Cosmogony of Super-Massive Black Holes;157
9.5.1;1 Introduction and Motivation;157
9.5.2;2 Black Hole Formation and Growth in Galactic Centers;157
9.5.3;3 Evolution of Self-Gravitating Accretion Disks and the Growth of Black Hole Masses;158
9.5.4;4 Discussion and Outlook;160
9.5.5;References;161
9.6;The Flare Activity of Sagittarius A*;162
9.6.1;1 Introduction;162
9.6.2;2 NIR/X-Ray Correlation;163
9.6.3;3 NIR Polarization Measurements;164
9.6.4;References;165
9.7;Mass Function of Remnant Black Holes in Nearby Galaxies;166
9.7.1;1 Overview;166
9.7.2;2 Previous results;166
9.7.3;3 Our sample;167
9.7.4;4 Preliminary results;167
9.7.5;References;168
9.8;Tidal Capture by a Black Hole and Flares in Galactic Centres;169
9.8.1;1 Introduction;169
9.8.2;2 Flares from a tidal disruption of a Solar type star by a 106M black hole;169
9.8.3;3 The time scale puzzle of flares in Sagittarius A* and tidal disruption and infall of a comet or asteroid;170
9.8.4;References;171
9.9;Low-Rate Accretion onto Isolated Stellar-Mass Black Holes;172
9.9.1;References;175
9.10;Clumps of material orbiting a black hole and the QPOs;177
9.10.1;1 Succesive passages of an asteroid about a black hole;177
9.10.2;2 Conclusions;178
9.10.3;References;179
9.11;Multi-Scale Simulations of Merging Galaxies with Supermassive Black Holes;180
9.11.1;1 Introduction;180
9.11.2;2 The Numerical Simulations;181
9.11.3;3 Gas Inflows and the Structure of the Nuclear Disks;182
9.11.4;4 Sinking SMBHs;183
9.11.5;5 Conclusions;183
9.11.6;References;184
9.12;The Parallel Lives of Supermassive Black Holes and their Host Galaxies;186
9.12.1;1 Introduction;186
9.12.2;2 SMBH as Tracers of Galaxy Evolution;188
9.12.3;3 Conclusions;190
9.12.4;References;190
9.13;The Polarization Properties of Sgr A* at Submillimeter Wavelengths;191
9.13.1;1 Introduction;191
9.13.2;2 The Submillimeter Array (SMA);192
9.13.3;3 Observations and Results;194
9.13.4;4 Discussion;195
9.13.5;5 Future Observations;196
9.13.6;References;196
9.14;Highlights of XMM-Newton Observations of Black Holes;198
9.14.1;1 Introduction;198
9.14.2;2 Birth of Black Holes;199
9.14.3;3 The Growing of Black Holes;199
9.14.4;4 Close to the Event-Horizon: Mass and Spin;199
9.14.5;5 Resum • e;201
9.14.6;References;201
9.15;Evolution of Supermassive Black Holes;202
9.15.1;1 Introduction;202
9.15.2;2 Sowing the Seeds of Black Holes;203
9.15.3;3 Spinning Top Toys and Yo-Yos;205
9.15.4;4 Playing Pools with Black Holes;207
9.15.5;5 Conclusions;208
9.15.6;References;208
10;Active Galactic Nuclei;211
10.1;AGN and XRB Variability: Propagating-Fluctuation Models;212
10.1.1;1 Introduction;212
10.1.2;2 Observed X-ray Timing Properties;212
10.1.3;3 Fluctuating Accretion Models;213
10.1.4;4 Fits to Real Data;214
10.1.5;References;215
10.2;The Source of Variable Optical Emission is Localized in the Jet of the Radio Galaxy 3C 390.3;216
10.2.1;1 The Link between Variable Radio Emission of the Jet and Optical Continuum Emission;216
10.2.2;2 The Central Sub-Pc-Scale Region in 3C 390.3;217
10.2.3;References;218
10.3;XMM-Newton RGS Spectra in Type 2 Seyfert Galaxies;219
10.4;First Results from the Extended Chandra Deep Field- South ( E- CDF- S) Survey;222
10.4.1;Pointers to the Refereed Scientific Literature;222
10.4.2;References;223
10.5;The Optical and X-ray Properties of AGN in COSMOS;224
10.5.1;1 The XMM-COSMOS Survey;224
10.5.2;2 Multicolor Properties of hard X-ray Sources;224
10.5.3;3 X-ray Spectral Properties;226
10.5.4;References;228
10.6;Relativistic Iron Lines at High Redshifts;229
10.6.1;1 Introduction;229
10.6.2;2 Stacking in XMMÒ;231
10.6.3;and;231
10.6.4;Deep Fields;231
10.6.5;3 Searching for Broad Lines in Deep Fields;231
10.6.6;4 Conclusions;233
10.6.7;References;233
10.7;An Explanation for the Soft X-Ray Excess in Active Galactic Nuclei;234
10.7.1;1 Introduction;234
10.7.2;2 Data & Analysis;235
10.7.3;3 Results & Discussion;236
10.7.4;References;238
10.8;Extended Inverse-Compton Emission from Distant, Powerful Radio Galaxies;239
10.8.1;1 Introduction;239
10.8.2;2 3C 432;239
10.8.3;3 3C 191;240
10.8.4;References;240
10.9;The Most Distant Radio Quasar as seen with the Highest Resolution;242
10.9.1;1 Introduction;242
10.9.2;2 Observations;242
10.9.3;3 Results and discussion;243
10.9.4;References;244
10.10;Investigating Narrow-Line Seyfert 1 with X-Ray Spectral Complexity;245
10.10.1;1 The high-energy spectral complexity in narrow-line Seyfert 1 galaxies;245
10.10.2;2 Sample definition;246
10.10.3;3 Results;246
10.10.4;References;247
10.11;A Survey of Gaussian Flares in AGN;248
10.11.1;1 Description of the study and motivation;248
10.11.2;2 Results;248
10.11.3;References;250
10.12;A Simple Model for Quasar Density Evolution;251
10.12.1;1 Introduction;251
10.12.2;2 Outline of the model;251
10.12.3;3 Results;252
10.12.4;References;253
10.13;The Dispersion of the MIR Ò Hard X-ray Correlation in AGN;254
10.13.1;1 Introduction;254
10.13.2;2 Our project and data;255
10.13.3;3 Conclusion;256
10.13.4;References;256
10.14;Gamma-Ray Probe of the QSOÌs Obscured Evolution;257
10.14.1;1 Obscured AGNs;257
10.14.2;2 Conclusions;259
10.14.3;References;259
10.15;Optical Observations of SBS1520+530 at TUG;260
10.15.1;1 Introduction;260
10.15.2;2 Observations and photometry;261
10.15.3;3 Results;262
10.15.4;References;262
10.16;Less is More? Are Radiogalaxies Below the Fanaroff- Riley Break More Polarised on Pc-Scales?;263
10.16.1;1 Introduction;263
10.16.2;2 Observations and Results;263
10.16.3;3 Conclusions;265
10.16.4;References;265
10.17;Relativistic Effects on the Observed AGN Luminosity Distribution and Spectral Shape of Seyfert Galaxies;266
10.17.1;1 Introduction;266
10.17.2;2 AGN Luminosity Distribution with Relativistic Corrections;266
10.17.3;3 X-Ray Spectra from Seyfert I and Seyfert II AGNs with Relativistic Corrections;267
10.17.4;4 Conclusion and Discussion;268
10.17.5;References;268
10.18;Nuclear Activity in Galaxies driven by Binary Supermassive Black Holes;269
10.18.1;1 Binary Black Holes and Nuclear Activity in Galaxies;269
10.18.2;2 Conclusion;272
10.18.3;References;273
10.19;Extragalactic Photon Background above GeV Energies: High Peaked BL Lacertae Objects or Dark Matter?;274
10.19.1;1 Introduction;274
10.19.2;2 Blazars detected with imaging air Cherenkov Telescopes;275
10.19.3;3 Gamma Rays due to annihilating SUSY Dark Matter;277
10.19.4;4 Comparison of astrophysical and combined EGRB Models;279
10.19.5;References;280
10.20;Resolving the Dust Tori in AGN with the VLT Interferometer;281
10.20.1;1 Dust Tori in AGN: what do we expect ?;281
10.20.2;2 The Seyfert II Case: Resolving the Torus;282
10.20.3;3 A Special Case: the Radio Galaxy Centaurus A;284
10.20.4;4 First Conclusions;285
10.20.5;References;286
10.21;Iron K Lines of AGN in the XÒRay Background;288
10.21.1;1 XÒRay Deep Field Observations of the Lockman Hole;288
10.21.2;2 Model of the Iron K Line Features;288
10.21.3;3 Conclusions;290
10.21.4;References;290
10.22;Black Hole Mass and Growth Rate and Metal Enrichment at Low and High Redshift;291
10.22.1;1 Introduction;291
10.22.2;2 Mass Accretion Rate and Metallicity at High Redshift;292
10.22.3;3 Mass Accretion Rate and Metallicity at Low Redshift;292
10.22.4;Log;293
10.22.5;N V/ C IV;293
10.22.6;4 Growth Time of Massive Black Holes and Time Dependent Metallicity;295
10.22.7;5 Conclusions;297
10.22.8;References;297
10.23;Is the Light Bending Effect atWork in the Core of NGC 4051?;299
10.23.1;References;301
10.24;Jet Activity in Supermassive Binary Black Holes;303
10.24.1;1 Introduction;303
10.24.2;2 Periodic Variability in Close SBBHs;303
10.24.3;3 Jet Activity and Evolution of SBBHs;305
10.24.4;References;305
10.25;Statistics of Local Hard X-Ray Selected AGN: Contribution of Obscured Accretion Onto Supermassive Black Holes;306
10.25.1;1 Introduction;306
10.25.2;2 RXTE Slew Survey (XSS) at 3Ò20 keV;306
10.25.3;3 INTEGRAL All-Sky Survey above 20 keV;307
10.25.4;4 Conclusion;307
10.25.5;References;309
10.26;3D-Models of Clumpy Tori in Seyfert Galaxies;310
10.26.1;1 Introduction;310
10.26.2;2 Our Model;310
10.26.3;3 Dust: Mass Study;311
10.26.4;4 Conclusions;312
10.26.5;References;312
11;Clusters of Galaxies;314
11.1;Cosmological Tests with Galaxy Clusters;315
11.1.1;1 Introduction;315
11.1.2;2 Cosmological Tests with the Abundance and Spatial Distribution of Clusters;316
11.1.3;3 Complementarity to other Cosmological Tests and Conclusions;318
11.1.4;References;319
11.2;Supermassive Black Holes in Elliptical Galaxies: Switching from Very Bright to Very Dim;321
11.2.1;1 Introduction;321
11.2.2;2 Black Hole Energy Release in X-ray Binaries and AGNs;322
11.2.3;3 Conclusions;325
11.2.4;References;325
11.3;Metal Enrichment of the ICM due to Ram-Pressure Stripping of Cluster Galaxies;326
11.3.1;1 Introduction;326
11.3.2;2 Numerical Method;326
11.3.3;3 Results;328
11.3.4;References;328
11.4;Radio Bubbles in Clusters: Relativistic Particle Content;329
11.4.1;1 Introduction;329
11.4.2;2 ParticleEnergies;329
11.4.3;3 Jet Matter Content;330
11.4.4;4 Conclusions;331
11.4.5;References;331
11.5;The XMM-Newton Distant Cluster Project;333
11.5.1;1 Introduction;333
11.5.2;2 The XMM-Newton Distant Cluster Project;333
11.5.3;References;335
11.6;Tracing the MassÒAssembly History of Galaxies with Deep Surveys;336
11.6.1;1 Introduction;336
11.6.2;2 Connecting Star Formation and Stellar Mass;336
11.6.3;3 The Build-up of the Most Massive Galaxies;337
11.6.4;References;338
11.7;Outbursts from Supermassive Black Holes and their Impacts on the Hot Gas in Early- Type Galaxies, Groups and Clusters;340
11.7.1;1 Hot Gas in Early Type Galaxies, Groups, and Clusters;340
11.7.2;2 M87 - A CANONICAL CLUSTER COOLING CORE;341
11.7.3;3 Hot Gas in Early Type Galaxies, Groups, and Clusters;344
11.7.4;4 Conclusion;344
11.7.5;References;345
11.8;Tracing Gas Motions in the Centaurus Cluster;346
11.8.1;1 Introduction;346
11.8.2;2 Model;346
11.8.3;3 Results;346
11.8.4;4 Turbulent Heating;348
11.8.5;References;348
11.9;Simulations of GalacticWinds and Starbursts in Galaxy Clusters;349
11.9.1;1 Introduction;349
11.9.2;2 Numerical methods;349
11.9.3;3 Summary and Conclusions;351
11.9.4;References;351
11.10;The ARCRAIDER Project: A Unique Sample of X-Ray Bright, Massive Gravitational Lensing Galaxy Clusters;352
11.10.1;1 Introduction;352
11.10.2;2 Optical Observations of Z3146;352
11.10.3;3 Lensing Analysis;353
11.10.4;4 X-ray Analysis;354
11.10.5;5 Conclusions;355
11.10.6;References;355
11.11;APEX-SZ: A Sunyaev-ZelÌdovich Galaxy Cluster Survey;357
11.11.1;1 Motivation for SZ cluster surveys;357
11.11.2;2 An SZ receiver for the APEX telescope;357
11.11.3;3 Expected galaxy cluster sample;358
11.11.4;4 Scientific goals of the APEX-SZ survey;358
11.11.5;5 First light observations;358
11.11.6;6 Conclusions;359
11.11.7;References;359
11.12;Detecting Virialization Shocks Around Galaxy Clusters Through the SZ Effect;360
11.12.1;1 Overview;360
11.12.2;2 Cluster profiles;360
11.12.3;3 Significance of detecting shocks;361
11.12.4;4 Parameter estimation;361
11.12.5;References;362
11.13;Numerical Simulations of Metal Enrichment and Mergers in Clusters of Galaxies;363
11.13.1;1 Introduction;363
11.13.2;2 The Simulations;363
11.13.3;3 Tracing Gas in Cluster Mergers;364
11.13.4;4 Metal Enrichment of the Intra-Cluster Medium;364
11.13.5;References;365
11.14;Turbulence in Galaxy Clusters: Impact on the Abundance Profiles;366
11.14.1;1 Introduction;366
11.14.2;2 The Model;366
11.14.3;3 Results;368
11.14.4;References;369
11.15;Studying the Nature of Dark Energy with Galaxy Clusters;370
11.15.1;1 Introduction;370
11.15.2;2 Local Cluster Sample;370
11.15.3;3 Distant Cluster Sample;372
11.15.4;References;373
11.16;Hydrodynamical Simulations of Cluster Formation with Central AGN Heating;375
11.16.1;1 Method;375
11.16.2;2 AGN Heating in Isolated Halos;375
11.16.3;3 AGN Feedback in Cosmological Simulations;377
11.16.4;4 Conclusions;377
11.16.5;References;378
11.17;Metal Enrichment Processes in the Intra-Cluster Medium;379
11.17.1;1 Introduction;379
11.17.2;2 Numerical Method;380
11.17.3;3 Results;380
11.17.4;4 Outlook;382
11.17.5;References;382
11.18;Ultraviolet-Bright, High-Redshift ULIRGS;384
11.18.1;1 Introduction;384
11.18.2;2 Observations and Analysis;385
11.18.3;3 Ultraviolet-Bright ULIRGs;385
11.18.4;References;388
12;Gamma Ray Bursts;389
12.1;The Correlation between .F. Peak Energy and radiated Energy in GammaÒ Ray Bursts;390
12.1.1;1 Introduction;390
12.1.2;2 TheE;391
12.1.3;Ò E;391
12.1.4;correlation: observations;391
12.1.5;3 Main implications of the E;392
12.1.6;Ò E;392
12.1.7;correlation;392
12.1.8;References;395
12.2;Particle Acceleration and Radiative Losses at Relativistic Shocks;396
12.2.1;1 Background and Methods;396
12.2.2;2 Results;397
12.2.3;References;398
12.3;The Swift Gamma-Ray Burst Mission: First Results;400
12.3.1;1 INTRODUCTION;400
12.3.2;2 SWIFT HIGHLIGHTS;401
12.3.3;3 CONCLUSIONS;407
12.3.4;References;407
12.4;The Afterglow of the Gamma-Ray Burst 050502a: First Case of an Early (< 1 hr) MultiÒ Colour Detection;409
12.4.1;1 Introduction;409
12.4.2;2 GRB 050502a: first early multi-colour light curve;410
12.4.3;References;411
12.5;Kinetic Plasma Simulations of GRB Fireball Collisions: Synchrotron Features;413
12.5.1;GRB polarimetry: Constraints on fireball models;413
12.5.2;Turbulent magnetic fields and synchrotron emission;413
12.5.3;References;415
12.6;Relativistic Jet Propagation in the Progenitor of GRBs;416
12.6.1;1 Introduction;416
12.6.2;2 Model and Numerical Method;416
12.6.3;3 Results and Discussion;417
12.6.4;4 Summary;418
12.6.5;References;418
12.7;Gravitational Collapse and Neutrino Emission of Population III Massive Stars;419
12.7.1;1 Introduction;419
12.7.2;2 Models and Methods;420
12.7.3;3 Gravitational Collapse of Pop III Massive Stars;420
12.7.4;4 Relic Neutrino from Pop III Massive Stars;420
12.7.5;5 Conclusions;422
12.7.6;References;423
12.8;Theoretical Interpretation of GRB 031203 and URCA-3;424
12.8.1;1 Luminosity and Spectral Properties.;424
12.8.2;2 The GRB 031203/Sn2003lw/URCA-3 Connection.;425
12.8.3;References;426
12.9;Baryonic Loading and e+ e- Rate Equation in GRB Sources;427
12.9.1;1 Introduction;427
12.9.2;2 Contrasts in the Dynamical Description of the Expanding Plasma;428
12.9.3;3 Conclusions;428
12.9.4;References;430
12.10;Gamma-ray Bursts from X-ray Binaries;432
12.10.1;1 Introduction;432
12.10.2;2 Magnetization of LMXBs;432
12.10.3;3 Generation of Differential Rotation;433
12.10.4;4 Open Issues;434
12.10.5;References;434
13;X-ray Binaries and Jets;436
13.1;Accretion and Relativistic Jets in Galactic Microquasars;437
13.1.1;1 Introduction;437
13.1.2;2 Source States in a Nutshell;437
13.1.3;3 Time Variability as a Tracer;438
13.1.4;4 Conclusions: Noisy Accretion and Ejection;440
13.1.5;References;441
13.2;Spectral and Variability Properties of LS 5039 from Radio to very High- Energy Gamma- Rays;442
13.2.1;1 Introduction;442
13.2.2;2 A Cold Matter Dominated Jet Model applied to LS 5039;442
13.2.3;References;443
13.3;30 Years Blandford-Znajek Process Ò Are Black Hole Jets Driven by the Ergosphere ?;446
13.3.1;1 The Two Hairs of Black Holes;446
13.3.2;2 Black Hole Magnetospheres;449
13.3.3;3 TimeÒDependent GRMHD and Jet Outflows;449
13.3.4;References;450
13.4;Radiative Acceleration and Collimation of Jets from TCAF Discs;452
13.4.1;1 Introduction;452
13.4.2;2 Model Assumptions and Results;452
13.4.3;3 Conclusion;454
13.4.4;References;454
13.5;Relativistic Jets in Active Galactic Nuclei: Importance of Magnetic Fields;455
13.5.1;1 Power of the Jets Launching;455
13.5.2;2 Efficiency of the Jet Launching;457
13.5.3;3 Conclusions;457
13.5.4;References;457
13.6;String Mechanism for Relativistic Jet Formation;458
13.6.1;References;460
13.7;Shock Location in Funnel Flows onto Magnetized Neutron Stars;461
13.7.1;References;464
13.8;General Relativistic Simulation of Jet Formation in Kerr Black Hole Magnetosphere;465
13.8.1;1 Introduction;465
13.8.2;2 Results;466
13.8.3;3 Conclusion;468
13.8.4;References;468
13.9;Radio Jets as Decelerating Relativistic Flows;469
13.9.1;References;471
13.10;Extragalactic Relativistic Jets and Nuclear Regions in Galaxies;473
13.10.1;1 Introduction;473
13.10.2;2 Anatomy of Jets;474
13.10.3;3 Jets and Nuclear Regions in AGN;475
13.10.4;4 Conclusion;476
13.10.5;References;476
13.11;Modeling the Relativistic Jets in SS 433 Using Chandra X- ray Spectroscopy;478
13.11.1;1 Introduction;478
13.11.2;2 Observations;481
13.11.3;3 Preliminary Results;481
13.11.4;4 FurtherWork;482
13.11.5;References;482
13.12;General Relativistic MHD Simulations of Relativistic Jets from a Rotating Black Hole Magnetosphere;483
13.12.1;1 Simulations;483
13.12.2;2 Results;484
13.12.3;3 Summary and Discussion;484
13.12.4;References;485
13.13;Particle Acceleration, Magnetic Field Generation, and Emission in Relativistic Pair Jets withWeibel Instability;486
13.13.1;1 Simulations;486
13.13.2;2 Summary and Discussion;488
13.13.3;References;488
13.14;Analytical and Numerical Studies of Fluid Instabilities in Relativistic Jets;489
13.14.1;1 Introduction;489
13.14.2;2 Numerical Simulations;490
13.14.3;References;491
13.15;Forced Oscillations in Relativistic Accretion Disks and QPOs;492
13.15.1;1 Introduction;492
13.15.2;2 Hydrodynamical Disk [3];492
13.15.3;3 Slow vs Fast Rotator;493
13.15.4;4 Conclusion;494
13.15.5;References;494
13.16;QPOs: EinsteinÌs Gravity Non-Linear Resonances;495
13.16.1;1 Introduction;495
13.16.2;2 QPOs and General Relativity;495
13.16.3;3 Klu • zniak-Abramowicz Resonance Model;496
13.16.4;4 Conclusions;498
13.16.5;References;498
13.17;Cosmic-Ray Acceleration and Viscosity;501
13.17.1;1 Introduction;501
13.17.2;2 Cosmic-Ray Acceleration in Shear Flows;501
13.17.3;3 Cosmic-Ray Viscosity;502
13.17.4;References;503
13.18;Gamma-Ray Emission from Microquasars: Leptonic vs. Hadronic Models;504
13.18.1;1 Introduction;504
13.18.2;2 A Leptonic Model for Microquasars;505
13.18.3;3 A Hadronic Model for Microquasars;505
13.18.4;4 Discussion;506
13.18.5;References;506
13.19;Magnetized Supernovae and Pulsar Recoils;507
13.19.1;1 Introduction;507
13.19.2;2 Models;507
13.19.3;3 Results;508
13.19.4;4 Discussion and Conclusion;508
13.19.5;5 Acknowledgments;508
13.19.6;References;510
13.20;Jet Deceleration: the Case of PKS 1136-135;511
13.20.1;1 Introduction;511
13.20.2;2 Modelling Deceleration;511
13.20.3;3 Discussion;513
13.20.4;References;513
13.21;Some Conclusions on The Magnetic Fields of Neutron Stars in Atoll and Z Sources;514
13.21.1;1 Introduction;514
13.21.2;References;516
14;Conference Summary;517
15;EinsteinÌs Legacy: a Summary;518
16;Author Index;523