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| List of tables | |
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| List of figures | |
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| Preface | |
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| Overview | |
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| Where do we stand? | |
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| Why does anyone care? | |
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| Stellar evolution | |
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| Nuclear energy generation and neutrino fluxes | |
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| Uncertainties in the predictions | |
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| Experiments are required for progress | |
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| The [superscript 37]Cl experiment | |
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| The Kamiokande II experiment | |
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| A geochemical experiment: [superscript 98]Mo | |
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| Gallium detectors | |
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| Next-generation experiments | |
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| Electronic detection of pp neutrinos | |
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| Coherent scattering detectors | |
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| Some explanations of the solar neutrino problem | |
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| Discriminating among explanations | |
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| The next decade | |
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| Questions and answers | |
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| Stellar structure and evolution | |
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| Life history of a star | |
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| Basic equations | |
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| Principal results | |
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| Present status | |
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| Nuclear fusion reactions | |
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| The essentials | |
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| Reaction rates | |
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| The pp chain | |
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| Neutrino fluxes and terminations of the pp chain | |
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| The CNO cycle | |
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| Energy generation | |
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| What remains to be done? | |
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| The standard solar model | |
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| The input parameters | |
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| General method | |
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| Some characteristics of the standard solar model | |
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| Helioseismology | |
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| Nonstandard solar models | |
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| The low Z model | |
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| Iron precipitation | |
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| A burnt-out core | |
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| Rapid rotation | |
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| A strong magnetic field | |
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| A mixed-up Sun | |
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| Turbulent diffusion | |
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| Thermal instabilities | |
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| Hydrodynamic phenomena | |
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| [superscript 3]He instability | |
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| Massive mass loss | |
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| A central black hole | |
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| WIMPs | |
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| Q-nuclei | |
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| Non-Maxwellian velocity distribution | |
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| No [superscript 8]B produced or S[subscript 34] = 0 | |
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| CNO reaction dominant | |
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| The neutrinos | |
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| The neutrino-producing reactions | |
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| Information content | |
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| Neutrino energy spectra | |
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| Solar neutrino fluxes | |
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| Fluxes from other stars | |
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| Theoretical uncertainties | |
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| Logic | |
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| Examples | |
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| Neutrino cross sections | |
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| Power-law dependences | |
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| Monte Carlo simulations | |
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| Principal uncertainties | |
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| Neutrino cross sections | |
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| Absorption cross sections | |
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| Neutrino-electron scattering cross sections | |
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| Neutral currents | |
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| Beyond the standard model of electroweak interactions | |
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| Vacuum oscillations | |
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| Matter oscillations | |
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| Neutrino magnetic moment | |
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| Neutrino decay | |
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| WIMPs | |
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| Ockham's razor | |
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| The [superscript 37]Cl experiment | |
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| Standard model predictions | |
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| The experiment | |
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| The results | |
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| Theory versus experiment: the implications | |
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| Do solar neutrino fluxes vary with time? | |
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| Recent data | |
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| The future of the [superscript 37]Cl experiment | |
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| The [superscript 71]Ga experiments | |
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| Predictions of the standard model | |
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| The experiments | |
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| What can be learned? | |
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| Geochemical and radiochemical detectors: Mo, Tl, Li, Br, I | |
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| [superscript 98]Mo | |
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| [superscript 205]Tl | |
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| [superscript 7]Li | |
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| [superscript 81]Br | |
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| [superscript 127]I | |
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| Neutrino-electron scattering experiments | |
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| Water detectors | |
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| Kamiokande II | |
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| SUNLAB | |
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| LVD | |
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| Super Kamiokande: water | |
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| Sudbury neutrino observatory: deuterium | |
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| ICARUS I: liquid argon | |
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| Low-temperature detectors | |
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| Direct counting experiments | |
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| SNO: D[subscript 2]O | |
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| ICARUS: [superscript 40]Ar | |
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| [superscript 115]In | |
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| BOREX: [superscript 11]B | |
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| [superscript 19]F | |
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| Coherent scattering detectors | |
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| Stellar collapse | |
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| How a star gets into trouble | |
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| Neutrino emission from a standard stellar collapse | |
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| Neutrino bombs: how often and where? | |
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| Neutrinos from other galaxies | |
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| SN1987A | |
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| Expected number of events in detectors | |
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| Synopsis and future directions | |
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| What is needed | |
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| Solar neutrino detectors | |
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| Stellar collapses | |
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| Stellar evolution | |
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| Nuclear physics | |
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| Particle physics | |
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| The bottom line | |
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| An account of the development of the solar neutrino problem, John N. Bahcall and Raymond Davis, Jr. | |
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| References | |
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| Index | |