| List of tables | p. xii |
| List of figures | p. xv |
| Preface | p. xix |
| Overview | p. 1 |
| Where do we stand? | p. 3 |
| Why does anyone care? | p. 4 |
| Stellar evolution | p. 5 |
| Nuclear energy generation and neutrino fluxes | p. 10 |
| Uncertainties in the predictions | p. 13 |
| Experiments are required for progress | p. 17 |
| The [superscript 37]Cl experiment | p. 17 |
| The Kamiokande II experiment | p. 20 |
| A geochemical experiment: [superscript 98]Mo | p. 21 |
| Gallium detectors | p. 22 |
| Next-generation experiments | p. 24 |
| Electronic detection of pp neutrinos | p. 26 |
| Coherent scattering detectors | p. 27 |
| Some explanations of the solar neutrino problem | p. 28 |
| Discriminating among explanations | p. 32 |
| The next decade | p. 32 |
| Questions and answers | p. 32 |
| Stellar structure and evolution | p. 43 |
| Life history of a star | p. 44 |
| Basic equations | p. 46 |
| Principal results | p. 48 |
| Present status | p. 53 |
| Nuclear fusion reactions | p. 55 |
| The essentials | p. 56 |
| Reaction rates | p. 59 |
| The pp chain | p. 63 |
| Neutrino fluxes and terminations of the pp chain | p. 67 |
| The CNO cycle | p. 71 |
| Energy generation | p. 72 |
| What remains to be done? | p. 73 |
| The standard solar model | p. 77 |
| The input parameters | p. 80 |
| General method | p. 85 |
| Some characteristics of the standard solar model | p. 89 |
| Helioseismology | p. 104 |
| Nonstandard solar models | p. 113 |
| The low Z model | p. 115 |
| Iron precipitation | p. 116 |
| A burnt-out core | p. 117 |
| Rapid rotation | p. 118 |
| A strong magnetic field | p. 119 |
| A mixed-up Sun | p. 120 |
| Turbulent diffusion | p. 124 |
| Thermal instabilities | p. 125 |
| Hydrodynamic phenomena | p. 126 |
| [superscript 3]He instability | p. 127 |
| Massive mass loss | p. 129 |
| A central black hole | p. 131 |
| WIMPs | p. 133 |
| Q-nuclei | p. 136 |
| Non-Maxwellian velocity distribution | p. 137 |
| No [superscript 8]B produced or S[subscript 34] = 0 | p. 139 |
| CNO reaction dominant | p. 140 |
| The neutrinos | p. 143 |
| The neutrino-producing reactions | p. 144 |
| Information content | p. 146 |
| Neutrino energy spectra | p. 153 |
| Solar neutrino fluxes | p. 157 |
| Fluxes from other stars | p. 165 |
| Theoretical uncertainties | p. 169 |
| Logic | p. 171 |
| Examples | p. 173 |
| Neutrino cross sections | p. 178 |
| Power-law dependences | p. 182 |
| Monte Carlo simulations | p. 187 |
| Principal uncertainties | p. 191 |
| Neutrino cross sections | p. 193 |
| Absorption cross sections | p. 195 |
| Neutrino-electron scattering cross sections | p. 214 |
| Neutral currents | p. 240 |
| Beyond the standard model of electroweak interactions | p. 245 |
| Vacuum oscillations | p. 247 |
| Matter oscillations | p. 258 |
| Neutrino magnetic moment | p. 284 |
| Neutrino decay | p. 292 |
| WIMPs | p. 295 |
| Ockham's razor | p. 299 |
| The [superscript 37]Cl experiment | p. 301 |
| Standard model predictions | p. 303 |
| The experiment | p. 307 |
| The results | p. 316 |
| Theory versus experiment: the implications | p. 320 |
| Do solar neutrino fluxes vary with time? | p. 326 |
| Recent data | p. 337 |
| The future of the [superscript 37]Cl experiment | p. 339 |
| The [superscript 71]Ga experiments | p. 343 |
| Predictions of the standard model | p. 344 |
| The experiments | p. 347 |
| What can be learned? | p. 356 |
| Geochemical and radiochemical detectors: Mo, Tl, Li, Br, I | p. 363 |
| [superscript 98]Mo | p. 364 |
| [superscript 205]Tl | p. 370 |
| [superscript 7]Li | p. 372 |
| [superscript 81]Br | p. 374 |
| [superscript 127]I | p. 377 |
| Neutrino-electron scattering experiments | p. 379 |
| Water detectors | p. 381 |
| Kamiokande II | p. 384 |
| SUNLAB | p. 392 |
| LVD | p. 394 |
| Super Kamiokande: water | p. 396 |
| Sudbury neutrino observatory: deuterium | p. 396 |
| ICARUS I: liquid argon | p. 397 |
| Low-temperature detectors | p. 398 |
| Direct counting experiments | p. 401 |
| SNO: D[subscript 2]O | p. 402 |
| ICARUS: [superscript 40]Ar | p. 408 |
| [superscript 115]In | p. 412 |
| BOREX: [superscript 11]B | p. 416 |
| [superscript 19]F | p. 416 |
| Coherent scattering detectors | p. 418 |
| Stellar collapse | p. 421 |
| How a star gets into trouble | p. 423 |
| Neutrino emission from a standard stellar collapse | p. 428 |
| Neutrino bombs: how often and where? | p. 433 |
| Neutrinos from other galaxies | p. 437 |
| SN1987A | p. 438 |
| Expected number of events in detectors | p. 457 |
| Synopsis and future directions | p. 461 |
| What is needed | p. 461 |
| Solar neutrino detectors | p. 463 |
| Stellar collapses | p. 469 |
| Stellar evolution | p. 471 |
| Nuclear physics | p. 476 |
| Particle physics | p. 479 |
| The bottom line | p. 484 |
| An account of the development of the solar neutrino problem, John N. Bahcall and Raymond Davis, Jr. | p. 487 |
| References | p. 531 |
| Index | p. 555 |
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