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Neutrino Astrophysics

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ISBN-10: 052137975X

ISBN-13: 9780521379755

Edition: 1989

Authors: John N. Bahcall

List price: $59.99
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This authoritative text provides a lively, thought-provoking and informative summary of neutrino astrophysics. Neutrino astronomy is being revolutionized by the availability of new observational facilities. Theoretical work in astrophysics and in particle physics in increasing rapidly. The subject of solar neutrinos has many seemingly independent aspects, both in its theoretical basis (involving nuclear, atomic, and particle physics, geochemistry, and astronomy). For many physicists, solar neutrinos constitute the low-energy frontier of high-energy physics. Results from all these disciplines are combined here, providing a timely and unified discussion of the field. Each chapter begins with…    
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Book details

List price: $59.99
Copyright year: 1989
Publisher: Cambridge University Press
Publication date: 7/28/1989
Binding: Paperback
Pages: 592
Size: 5.98" wide x 8.98" long x 1.46" tall
Weight: 1.738
Language: English

List of tables
List of figures
Where do we stand?
Why does anyone care?
Stellar evolution
Nuclear energy generation and neutrino fluxes
Uncertainties in the predictions
Experiments are required for progress
The [superscript 37]Cl experiment
The Kamiokande II experiment
A geochemical experiment: [superscript 98]Mo
Gallium detectors
Next-generation experiments
Electronic detection of pp neutrinos
Coherent scattering detectors
Some explanations of the solar neutrino problem
Discriminating among explanations
The next decade
Questions and answers
Stellar structure and evolution
Life history of a star
Basic equations
Principal results
Present status
Nuclear fusion reactions
The essentials
Reaction rates
The pp chain
Neutrino fluxes and terminations of the pp chain
The CNO cycle
Energy generation
What remains to be done?
The standard solar model
The input parameters
General method
Some characteristics of the standard solar model
Nonstandard solar models
The low Z model
Iron precipitation
A burnt-out core
Rapid rotation
A strong magnetic field
A mixed-up Sun
Turbulent diffusion
Thermal instabilities
Hydrodynamic phenomena
[superscript 3]He instability
Massive mass loss
A central black hole
Non-Maxwellian velocity distribution
No [superscript 8]B produced or S[subscript 34] = 0
CNO reaction dominant
The neutrinos
The neutrino-producing reactions
Information content
Neutrino energy spectra
Solar neutrino fluxes
Fluxes from other stars
Theoretical uncertainties
Neutrino cross sections
Power-law dependences
Monte Carlo simulations
Principal uncertainties
Neutrino cross sections
Absorption cross sections
Neutrino-electron scattering cross sections
Neutral currents
Beyond the standard model of electroweak interactions
Vacuum oscillations
Matter oscillations
Neutrino magnetic moment
Neutrino decay
Ockham's razor
The [superscript 37]Cl experiment
Standard model predictions
The experiment
The results
Theory versus experiment: the implications
Do solar neutrino fluxes vary with time?
Recent data
The future of the [superscript 37]Cl experiment
The [superscript 71]Ga experiments
Predictions of the standard model
The experiments
What can be learned?
Geochemical and radiochemical detectors: Mo, Tl, Li, Br, I
[superscript 98]Mo
[superscript 205]Tl
[superscript 7]Li
[superscript 81]Br
[superscript 127]I
Neutrino-electron scattering experiments
Water detectors
Kamiokande II
Super Kamiokande: water
Sudbury neutrino observatory: deuterium
ICARUS I: liquid argon
Low-temperature detectors
Direct counting experiments
SNO: D[subscript 2]O
ICARUS: [superscript 40]Ar
[superscript 115]In
BOREX: [superscript 11]B
[superscript 19]F
Coherent scattering detectors
Stellar collapse
How a star gets into trouble
Neutrino emission from a standard stellar collapse
Neutrino bombs: how often and where?
Neutrinos from other galaxies
Expected number of events in detectors
Synopsis and future directions
What is needed
Solar neutrino detectors
Stellar collapses
Stellar evolution
Nuclear physics
Particle physics
The bottom line
An account of the development of the solar neutrino problem, John N. Bahcall and Raymond Davis, Jr.