Unsolved Problems in Astrophysics

Name: Unsolved Problems in Astrophysics
Brand: Princeton University Press
Price: 93.99 EUR
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John Bahcall Jeremiah P. Ostriker(Herausgeber*in)

Princeton University Press

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Erschienen am 5. Juni 2018

382 Seiten

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Inhalt

Cover
Title Page
Copyright Page
Contents
PREFACE
1 THE COSMOLOGICAL PARAMETERS
1.1 INTRODUCTION
1.2 WHY MEASURE THE PARAMETERS?
1.2.1 Testing the Physics
1.2.2 How Will It All End?
1.3 THE STATE OF THE MEASUREMENTS
1.4 COSMOLOGY FOR THE NEXT GENERATION
2 IN THE BEGINNING
2.1 THE FUTURE FATE OF COSMOLOGY
2.2 TESTING INFLATION
2.3 THE POWER OF THE COSMIC MICROWAVE BACKGROUND
2.4 COSMIC CONCORDANCE
2.5 A NEW AGE?
3 UNDERSTANDING DATA BETTER WITH BAYESIAN AND GLOBAL STATISTICAL METHODS
3.1 INTRODUCTION
3.2 COMBINING EXPERIMENTAL MEASUREMENTS
3.3 BAYESIAN COMBINATION OF INCOMPATIBLE MEASUREMENTS
3.4 ANOTHER VARIANT OF THE METHOD
3.5 RESULTS FOR THE HUBBLE CONSTANT
3.6 CONCLUSION
4 LARGE-SCALE STRUCTURE IN THE UNIVERSE
4.1 INTRODUCTION
4.2 CLUSTERING AND LARGE-SCALE STRUCTURE
4.2.1 Galaxies and Large-Scale Structure
4.2.2 Clusters and Large-Scale Structure
4.3 PECULIAR MOTIONS ON LARGE SCALES
4.4 DARK MATTER AND BARYONS IN CLUSTERS OF GALAXIES
4.5 lsiîm & 1?
4.6 THE SDSS AND LARGE-SCALE STRUCTURE
4.6.1 The Sloan Digital Sky Survey
4.6.2 Clusters of Galaxies
4.7 SUMMARY
5 UNSOLVED PROBLEMS IN GRAVITATIONAL LENSING
5.1 INTRODUCTION
5.2 GRAVITATIONAL LENS OPTICS
5.3 THE PROBLEMS
5.3.1 How Old Is the Universe?
5.3.2 What Is the Shape of the Universe?
5.3.3 What Is the Large Scale Distribution of Matter?
5.3.4 How Are Rich Clusters of Galaxies Formed?
5.3.5 When Did Galaxies Form and How Did They Evolve?
5.3.6 How Big Are Galaxies?
5.3.7 Of What Are Galaxies Made?
5.3.8 How Big Are AGN Ultraviolet Emission Regions ?
5.4 HOW MANY MORE SURPRISES WILL GRAVITATIONAL LENSES PROVIDE?
6 WHAT CAN BE LEARNED FROM NUMERICAL SIMULATIONS OF COSMOLOGY
6.1 INTRODUCTION
6.2 SIMULATION METHODS
6.2.1 Specification of Models
6.2.2 Physical Processes and Numerical Methods
6.3 RESULTS: COMPARISON WITH OBSERVATIONS
6.3.1 Hot Components
6.3.2 Warm Components
6.3.3 Cold Condensed Components
6.4 CONCLUSIONS, PROSPECTS, AND MORE QUESTIONS
7 THE CENTERS OF ELLIPTICAL GALAXIES
7.1 INTRODUCTION
7.1.1 Black Holes and Quasars
7.1.2 The Sphere of Influence
7.1.3 Cores and Cusps
7.2 PHOTOMETRY
7.2.1 The Peebles-Young Model
7.3 KINEMATIC EVIDENCE FOR CENTRAL BLACK HOLES
7.4 PHYSICAL PROCESSES
7.5 SUMMARY
8 THE MORPHOLOGICAL EVOLUTION OF GALAXIES
8.1 INTRODUCTION
8.2 EARLY FORMATION OF MASSIVE ELLIPTICALS
8.3 SLOW EVOLUTION OF MASSIVE DISK GALAXIES
8.4 REDSHIFT SURVEYS AND THE DWARF-DOMINATED UNIVERSE
8.5 FAINT GALAXY MORPHOLOGIES FROM HST
8.6 CONCLUSIONS
9 QUASARS
9.1 QUASARS AND THE END OF THE 'DARK AGE'
9.2 THE RELATION OF AGN S TO THE CENTRAL BULGES OF GALAXIES
9.3 QUASARS AND THEIR REMNANTS: PROBES OF GENERAL RELATIVITY?
9.3.1 Dead Quasars in Nearby Galaxies
9.3.2 Do These Holes Have a Kerr Metric?
10 SOLAR NEUTRINOS: SOLVED AND UNSOLVED PROBLEMS
10.1 WHY STUDY SOLAR NEUTRINOS?
10.2 WHAT DOES THE COMBINED STANDARD MODEL TELL US ABOUT SOLAR NEUTRINOS?
10.2.1 The Combined Standard Model
10.2.2 The Solar Neutrino Spectrum
10.3 WHY ARE THE PREDICTED NEUTRINO FLUXES ROBUST?
10.4 WHAT ARE THE THREE SOLAR NEUTRINO PROBLEMS?
10.4.1 Calculated versus Observed Chlorine Rate
10.4.2 Incompatibility of Chlorine and Water (Kamiokande) Ex periments
10.4.3 Gallium Experiments: No Room for7 Be Neutrinos
10.5 WHAT HAVE WE LEARNED?
10.5.1 About Astronomy
10.5.2 About Physics
10.6 WHAT NEXT?
10.6.1 Solvable Problems in Physics
10.6.2 Solvable Problems in Astronomy
10.7 SUMMARY
11 PARTICLE DARK MATTER
11.1 INTRODUCTION: THREE ARGUMENTS FOR NON-BARYONIC DARK MATTER
11.2 THE CASE FOR NON-BARYONIC MATTER
11.2.1 We've Looked for Baryonic Dark Matter and Failed
11.2.2 We Can't Seem To Make the Observed Large-Scale Structure with Baryons
11.2.3 Dynamical Mass Is Much Larger than Big Bang Nucleosynthesis Allows
11.3 NEUTRINOS AS DARK MATTER
11.3.1 Detecting Massive Neutrinos
11.4 WIMPs
11.4.1 Searching for WIMPs
11.4.2 Indirect WIMP Detection
11.4.3 What Is To Be Done?
11.5 AXIONS
11.6 CONCLUSIONS
12 STARS IN THE MILKY WAY AND OTHER GALAXIES
12.1 INTRODUCTION
12.2 RECENT STAR COUNT RESULTS
12.3 MICROLENSING AND STAR COUNTS
12.4 DISK DARK MATTER: STILL A QUESTION
12.5 MYSTERY OF THE LONG EVENTS
12.6 PROPER MOTIONS FROM EROS II
12.7 PIXEL LENSING: STELLAR MASS FUNCTIONS IN OTHER GALAXIES
12.8 STAR FORMATION HISTORY OF THE UNIVERSE
12.9 CONCLUSIONS
13 SEARCHING FOR MACHOS WITH MICROLENSING
13.1 INTRODUCTION
13.2 THE GRAVITATIONAL MICROLENS
13.3 THE "MACHO FRACTION" IN THE GALACTIC HALO
13.4 THE EXPERIMENTAL SITUATION
13.5 NEXT GENERATION EXPERIMENTS
13.5.1 What Can Be Achieved from the Ground?
13.5.2 Observing Macho Parallax
13.6 WORKING ON GRAVITATIONAL MICROLENSING
13.7 SUMMARY
13.7.1 What We Know Now
13.7.2 What We Will Learn from Current Experiments
13.7.3 Next Generation Experiments
13.8 LATE BREAKING NEWS
14 GLOBALLY ASYMMETRIC SUPERNOVA
14.1 INTRODUCTION
14.1.1 Preamble
14.1.2 Evidence for Asymmetry
14.1.3 State of the Art
14.2 INSTABILITY DURING CORE COLLAPSE
14.2.1 Accomplishments
14.2.2 Future Directions
14.3 OVERSTABLE CORE G-MODES
14.3.1 Accomplishments
14.3.2 Future Directions
14.3.3 Turbulent Excitation of g-Modes
15 IN AND AROUND NEUTRON STARS
15.1 INTRODUCTION
15.2 SUPERFLUID-SUPERCONDUCTOR INTERACTIONS IN A NEUTRON STAR CORE
15.3 THE STELLAR CRUST
15.4 SPUN-UP NEUTRON STARS
15.5 SPINNING-DOWN RADIOPULSARS
15.6 GLITCHES OF RADIOPULSAR SPIN PERIODS
16 ACCRETION FLOWS AROUND BLACK HOLES
16.1 INTRODUCTION
16.2 X-RAYS AND 7-RAYS FROM ACCRETING BLACK HOLES
16.3 HOT ACCRETION FLOW MODELS
16.3.1 Corona Models
16.3.2 SLE Two-Temperature Model
16.3.3 Optically-Thin Advection-Dominated Model
16.4 DIRECTIONS FOR FUTURE RESEARCH
16.4.1 Unresolved Theoretical Issues
16.4.2 Clues from Observations of Black Hole XRBs
16.4.3 Black Holes versus Neutron Stars
16.5 CONCLUSION
17 THE HIGHEST ENERGY COSMIC RAYS
17.1 INTRODUCTION
17.2 REVIEW OF EXISTING DATA ON THE HIGHEST ENERGY COSMIC RAYS
17.3 ACCELERATION AND TRANSPORT OF THE COSMIC RAYS & 1019 EV
17.4 THE BIG EVENTS
17.5 THE AUGER PROJECT
17.6 WHAT CAN WE LEARN FROM TWO LARGE SURFACE ARRAYS?
17.7 SHOULD A STUDENT WORK ON THIS PROBLEM?
17.8 FINAL REMARK
18 TOWARD UNDERSTANDING GAMMA-RAY BURSTS
18.1 INTRODUCTION
18.2 OBSERVATIONS
18.2.1 Observational Open Questions
18.3 A BRIEF SUMMARY
18.4 WHERE?
18.5 How?
18.5.1 The Compactness Problem
18.5.2 Relativistic Motion
18.5.3 Slowing Down of Relativistic Particles
18.5.4 The Acceleration Mechanism?
18.6 WHAT?
18.6.1 What Do We Need from the Internal Engine?
18.6.2 Coincidences and Other Astronomical Hints
18.7 WHY?
18.8 CONCLUSIONS
18.9 SOME OPEN QUESTIONS

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