Stars as Laboratories for Fundamental Physics - MPP Theory Group

More documents

Recommendations

Info

Chapter 16 Neutrinos: The Bottom Line Most of the particle-physics arguments discussed in this book are closely related to neutrino physics because these particles play an important role in stellar evolution whether or not they have nonstandard properties. Besides a summary of some recent developments of standardneutrino astrophysics, a synthesis is attempted of what stars as neutrino laboratories have taught us about these elusive objects, and what one might reasonable hope to learn in the foreseeable future. 16.1 Standard Neutrinos The main theme of this book has been an attempt to extract information about the properties of neutrinos and other weakly interacting particles from the established properties of stars. However, even standard-model neutrinos (massless, no mixing, no exotic properties) play a significant role in astrophysics. There have been some recent developments in “standard-neutrino astrophysics” which deserve mention in a summary. It is now thought that neutrinos play an active role in supernovae besides carrying away the binding energy of the newborn neutron star (Chapter 11). In the delayed-explosion scenario they are crucial to revive the stalled shock wave which is supposed to expel the stellar mantle and envelope. Moreover, they have a strong impact on r-process nucleosynthesis which is thought to occur in the high-entropy region above the neutron star a few seconds after collapse. For both purposes it is crucial to calculate the SN “neutrino lightcurve” for the first seconds after collapse. Convection below the neutrino sphere and large-scale convective turnovers in the region between the neutron star and the shock wave are both important and need to be understood better on 568
Neutrinos: The Bottom Line 569 the basis of 2- and 3-dimensional hydrodynamic calculations which are only beginning to appear in the literature. In addition, however, the neutrino opacities must be calculated with greater reliability. In Chapter 4 the weaknesses of a naive calculation of the axial-vector opacities have been amply demonstrated. In my opinion, a far better understanding of the interaction rates of neutrinos with a hot nuclear medium is required before one can calculate a SN neutrino lightcurve (notably the duration of Kelvin-Helmholtz cooling) with a reasonable precision. Neutrinos presumably play a key role for the self-acceleration of neutron stars which are observed to have huge “kick velocities” (Sect. 11.5). The required anisotropic neutrino emission of 1−2% may be caused by temperature fluctuations on the neutrino sphere (convection!), or by magnetic-field induced anisotropies of the neutrino opacities. Of course, other phenomena may be responsible for anisotropic neutrino emission and for the kick velocities. For the first time ever neutrinos have been observed from a collapsing star (SN 1987A), confirming the expected signal behavior within the large uncertainties caused by the small number of observed events (Chapter 11). Neutrinos are routinely observed from the Sun—currently in four different detectors with three different spectral response characteristics (Chapter 10). At least three further detectors will soon take up operations. The measured solar neutrino spectrum differs significantly from theoretical predictions. This “solar neutrino problem” has no obvious “astrophysical solution” that would involve plausible variations of input parameters such as nuclear cross sections or photon opacities. Still, the gallium detectors SAGE and GALLEX have for the first time measured the dominant low-energy flux of pp neutrinos, confirming that the Sun cannot be completely different at its center from what had been thought. There is also some more benign news. The interest of some authors to apply the methods of finite temperature field theory to astrophysical problems has led to a new formulation of the photon dispersion relation in a plasma (Sect. 6.3). It helped to correct some “fossilized errors” in the literature on plasma neutrino emission (see also Appendix C.1). It may well be worthwhile to scrutinize other standard aspects of stellarevolution input physics that involve subtle dispersion or screening effects.
Page 1 and 2:
Georg G. Raffelt Stars as Laborator
Page 3 and 4:
Table of Contents Preface (xiv) Ack
Page 5 and 6:
Table of Contents vii 4.5 Neutrino
Page 7 and 8:
Table of Contents ix 8. Neutrino Os
Page 9 and 10:
Table of Contents xi 12. Radiative
Page 11 and 12:
Table of Contents xiii 16.3 New Int
Page 13 and 14:
Preface xv Second, particles from d
Page 15 and 16:
Preface xvii search for proton deca
Page 17 and 18:
Preface xix cuts of higher-order gr
Page 19 and 20:
Preface xxi quoted “astrophysical
Page 21 and 22:
Chapter 1 The Energy-Loss Argument
Page 23 and 24:
The Energy-Loss Argument 3 example
Page 25 and 26:
The Energy-Loss Argument 5 trinos,
Page 27 and 28:
The Energy-Loss Argument 7 As a sim
Page 29 and 30:
The Energy-Loss Argument 9 The most
Page 31 and 32:
The Energy-Loss Argument 11 against
Page 33 and 34:
The Energy-Loss Argument 13 ing M;
Page 35 and 36:
The Energy-Loss Argument 15 M ′ (
Page 37 and 38:
The Energy-Loss Argument 17 Table 1
Page 39 and 40:
The Energy-Loss Argument 19 ing to
Page 41 and 42:
The Energy-Loss Argument 21 scalars
Page 43 and 44:
Chapter 2 Anomalous Stellar Energy
Page 45 and 46:
Anomalous Stellar Energy Losses Bou
Page 47 and 48:
Page 49 and 50:
Page 51 and 52:
Page 53 and 54:
Page 55 and 56:
Page 57 and 58:
Page 59 and 60:
Page 61 and 62:
Page 63 and 64:
Page 65 and 66:
Page 67 and 68:
Page 69 and 70:
Page 71 and 72:
Page 73 and 74:
Page 75 and 76:
Page 77 and 78:
Page 79 and 80:
Page 81 and 82:
Page 83 and 84:
Page 85 and 86:
Page 87 and 88:
Page 89 and 90:
Page 91 and 92:
Page 93 and 94:
Page 95 and 96:
Page 97 and 98:
Page 99 and 100:
Page 101 and 102:
Page 103 and 104:
Page 105 and 106:
Page 107 and 108:
Page 109 and 110:
Chapter 3 Particles Interacting wit
Page 111 and 112:
Particles Interacting with Electron
Page 113 and 114:
Page 115 and 116:
Page 117 and 118:
Page 119 and 120:
Page 121 and 122:
Page 123 and 124:
Page 125 and 126:
Page 127 and 128:
Page 129 and 130:
Page 131 and 132:
Page 133 and 134:
Page 135 and 136:
Page 137 and 138:
Chapter 4 Processes in a Nuclear Me
Page 139 and 140:
Processes in a Nuclear Medium 119 t
Page 141 and 142:
Processes in a Nuclear Medium 121 f
Page 143 and 144:
Processes in a Nuclear Medium 123 F
Page 145 and 146:
Page 147 and 148:
Page 149 and 150:
Processes in a Nuclear Medium 129 v
Page 151 and 152:
Processes in a Nuclear Medium 131 4
Page 153 and 154:
Processes in a Nuclear Medium 133 i
Page 155 and 156:
Processes in a Nuclear Medium 135 H
Page 157 and 158:
Processes in a Nuclear Medium 137 I
Page 159 and 160:
Page 161 and 162:
Page 163 and 164:
Processes in a Nuclear Medium 143 i
Page 165 and 166:
Processes in a Nuclear Medium 145 s
Page 167 and 168:
Processes in a Nuclear Medium 147 E
Page 169 and 170:
Processes in a Nuclear Medium 149 a
Page 171 and 172:
Processes in a Nuclear Medium 151 T
Page 173 and 174:
Processes in a Nuclear Medium 153 r
Page 175 and 176:
Processes in a Nuclear Medium 155 4
Page 177 and 178:
Processes in a Nuclear Medium 157 I
Page 179 and 180:
Processes in a Nuclear Medium 159 t
Page 181 and 182:
Processes in a Nuclear Medium 161 A
Page 183 and 184:
Processes in a Nuclear Medium 163 R
Page 185 and 186:
Chapter 5 Two-Photon Coupling of Lo
Page 187 and 188:
Two-Photon Coupling of Low-Mass Bos
Page 189 and 190:
Page 191 and 192:
Page 193 and 194:
Page 195 and 196:
Page 197 and 198:
Page 199 and 200:
Page 201 and 202:
Page 203 and 204:
Page 205 and 206:
Page 207 and 208:
Page 209 and 210:
Page 211 and 212:
Page 213 and 214:
Chapter 6 Particle Dispersion and D
Page 215 and 216:
Particle Dispersion and Decays in M
Page 217 and 218:
Page 219 and 220:
Page 221 and 222:
Page 223 and 224:
Page 225 and 226:
Page 227 and 228:
Page 229 and 230:
Page 231 and 232:
Page 233 and 234:
Page 235 and 236:
Page 237 and 238:
Page 239 and 240:
Page 241 and 242:
Page 243 and 244:
Page 245 and 246:
Page 247 and 248:
Page 249 and 250:
Page 251 and 252:
Page 253 and 254:
Page 255 and 256:
Page 257 and 258:
Page 259 and 260:
Page 261 and 262:
Page 263 and 264:
Page 265 and 266:
Page 267 and 268:
Page 269 and 270:
Page 271 and 272:
Chapter 7 Nonstandard Neutrinos The
Page 273 and 274:
Nonstandard Neutrinos 253 (“spont
Page 275 and 276:
Nonstandard Neutrinos 255 kinematic
Page 277 and 278:
Nonstandard Neutrinos 257 95% CL ma
Page 279 and 280:
Nonstandard Neutrinos 259 Fig. 7.2.
Page 281 and 282:
Nonstandard Neutrinos 261 In three-
Page 283 and 284:
Nonstandard Neutrinos 263 Flavor mi
Page 285 and 286:
Page 287 and 288:
Nonstandard Neutrinos 267 The quant
Page 289 and 290:
Nonstandard Neutrinos 269 dipole mo
Page 291 and 292:
Nonstandard Neutrinos 271 component
Page 293 and 294:
Page 295 and 296:
Nonstandard Neutrinos 275 moments.
Page 297 and 298:
Nonstandard Neutrinos 277 7.5.2 Spi
Page 299 and 300:
Nonstandard Neutrinos 279 where m
Page 301 and 302:
Neutrino Oscillations 281 and hence
Page 303 and 304:
Neutrino Oscillations 283 As usual
Page 305 and 306:
Neutrino Oscillations 285 two-flavo
Page 307 and 308:
Neutrino Oscillations 287 Fig. 8.2.
Page 309 and 310:
Neutrino Oscillations 289 8.2.4 Exp
Page 311 and 312:
Page 313 and 314:
Neutrino Oscillations 293 Apparentl
Page 315 and 316:
Page 317 and 318:
Neutrino Oscillations 297 when the
Page 319 and 320:
Neutrino Oscillations 299 If the ne
Page 321 and 322:
Neutrino Oscillations 301 8.3.5 The
Page 323 and 324:
Neutrino Oscillations 303 It is als
Page 325 and 326:
Neutrino Oscillations 305 system, h
Page 327 and 328:
Neutrino Oscillations 307 say, betw
Page 329 and 330:
Neutrino Oscillations 309 1991). Th
Page 331 and 332:
Oscillations of Trapped Neutrinos 3
Page 333 and 334:
Page 335 and 336:
Page 337 and 338:
Page 339 and 340:
Page 341 and 342:
Page 343 and 344:
Page 345 and 346:
Page 347 and 348:
Page 349 and 350:
Page 351 and 352:
Page 353 and 354:
Page 355 and 356:
Page 357 and 358:
Page 359 and 360:
Page 361 and 362:
Chapter 10 Solar Neutrinos The curr
Page 363 and 364:
Solar Neutrinos 343 Fig. 10.1. Sola
Page 365 and 366:
Solar Neutrinos 345 There exist vas
Page 367 and 368:
Solar Neutrinos 347 10.2 Calculated
Page 369 and 370:
Solar Neutrinos 349 Fig. 10.3. Norm
Page 371 and 372:
Solar Neutrinos 351 a certain range
Page 373 and 374:
Solar Neutrinos 353 While helium an
Page 375 and 376:
Solar Neutrinos 355 Bahcall and Pin
Page 377 and 378:
Solar Neutrinos 357 Xu et al. (1994
Page 379 and 380:
Solar Neutrinos 359 Table 10.4. Spe
Page 381 and 382:
Solar Neutrinos 361 Table 10.5. Pre
Page 383 and 384:
Solar Neutrinos 363 rates attribute
Page 385 and 386:
Solar Neutrinos 365 10.3.4 Water Ch
Page 387 and 388:
Solar Neutrinos 367 Fig. 10.10. Dif
Page 389 and 390:
Solar Neutrinos 369 Fig. 10.13. Mea
Page 391 and 392:
Solar Neutrinos 371 Table 10.9. Cur
Page 393 and 394:
Solar Neutrinos 373 of order the an
Page 395 and 396:
Solar Neutrinos 375 Fig. 10.16. 37
Page 397 and 398:
Solar Neutrinos 377 GALLEX, or Home
Page 399 and 400:
Solar Neutrinos 379 Table 10.10. Me
Page 401 and 402:
Solar Neutrinos 381 deficits in all
Page 403 and 404:
Solar Neutrinos 383 The ν e surviv
Page 405 and 406:
Solar Neutrinos 385 The allowed ran
Page 407 and 408:
Solar Neutrinos 387 10.7 Spin and S
Page 409 and 410:
Solar Neutrinos 389 10.8 Neutrino D
Page 411 and 412:
Solar Neutrinos 391 The small- and
Page 413 and 414:
Solar Neutrinos 393 flux above its
Page 415 and 416:
Chapter 11 Supernova Neutrinos The
Page 417 and 418:
Supernova Neutrinos 397 Fig. 11.1.
Page 419 and 420:
Supernova Neutrinos 399 beyond the
Page 421 and 422:
Supernova Neutrinos 401 ate neutrin
Page 423 and 424:
Supernova Neutrinos 403 Convection
Page 425 and 426:
Supernova Neutrinos 405 Hayes, and
Page 427 and 428:
Supernova Neutrinos 407 11.2 Predic
Page 429 and 430:
Supernova Neutrinos 409 must then b
Page 431 and 432:
Supernova Neutrinos 411 Figure 11.6
Page 433 and 434:
Supernova Neutrinos 413 signal (Sec
Page 435 and 436:
Supernova Neutrinos 415 time) on 23
Page 437 and 438:
Supernova Neutrinos 417 All of the
Page 439 and 440:
Supernova Neutrinos 419 to multiple
Page 441 and 442:
Supernova Neutrinos 421 the final-s
Page 443 and 444:
Supernova Neutrinos 423 ter of 53 e
Page 445 and 446:
Supernova Neutrinos 425 Given these
Page 447 and 448:
Supernova Neutrinos 427 thorough st
Page 449 and 450:
Supernova Neutrinos 429 The forward
Page 451 and 452:
Supernova Neutrinos 431 Another int
Page 453 and 454:
Supernova Neutrinos 433 ber of ν e
Page 455 and 456:
Supernova Neutrinos 435 A “normal
Page 457 and 458:
Supernova Neutrinos 437 Fig. 11.19.
Page 459 and 460:
Supernova Neutrinos 439 The approxi
Page 461 and 462:
Supernova Neutrinos 441 be taken to
Page 463 and 464:
Supernova Neutrinos 443 sense that
Page 465 and 466:
Supernova Neutrinos 445 presence of
Page 467 and 468:
Supernova Neutrinos 447 An even mor
Page 469 and 470:
Chapter 12 Radiative Particle Decay
Page 471 and 472:
Radiative Particle Decays 451 one c
Page 473 and 474:
Radiative Particle Decays 453 corre
Page 475 and 476:
Radiative Particle Decays 455 is no
Page 477 and 478:
Radiative Particle Decays 457 Fig.
Page 479 and 480:
Page 481 and 482:
Radiative Particle Decays 461 12.3.
Page 483 and 484:
Radiative Particle Decays 463 emiss
Page 485 and 486:
Radiative Particle Decays 465 range
Page 487 and 488:
Page 489 and 490:
Radiative Particle Decays 469 weak
Page 491 and 492:
Radiative Particle Decays 471 value
Page 493 and 494:
Radiative Particle Decays 473 ignor
Page 495 and 496:
Page 497 and 498:
Page 499 and 500:
Radiative Particle Decays 479 Table
Page 501 and 502:
Radiative Particle Decays 481 In or
Page 503 and 504:
Page 505 and 506:
Radiative Particle Decays 485 while
Page 507 and 508:
Radiative Particle Decays 487 h 100
Page 509 and 510:
Page 511 and 512:
Radiative Particle Decays 491 still
Page 513 and 514:
Chapter 13 What Have We Learned fro
Page 515 and 516:
What Have We Learned from SN 1987A
Page 517 and 518:
Page 519 and 520:
Page 521 and 522:
Page 523 and 524:
Page 525 and 526:
Page 527 and 528:
Page 529 and 530:
Page 531 and 532:
Page 533 and 534:
Page 535 and 536:
Page 537 and 538: What Have We Learned from SN 1987A
Page 545 and 546: Axions 525 Table 14.1. Particle mag
Page 547 and 548: Axions 527 or axion decay constant.
Page 549 and 550: Axions 529 The Yukawa coupling h is
Page 551 and 552: Axions 531 14.2.3 Pseudoscalar vs.
Page 553 and 554: Axions 533 Notably, the Higgs field
Page 555 and 556: Axions 535 otic heavy quarks: only
Page 557 and 558: Axions 537 Various axion models dif
Page 559 and 560: Axions 539 Bounds on the Yukawa cou
Page 561 and 562: Axions 541 Fig. 14.5. Astrophysical
Page 563 and 564: Axions 543 decay into axions. This
Page 565 and 566: Chapter 15 Miscellaneous Exotica St
Page 567 and 568: Miscellaneous Exotica 547 Table 15.
Page 569 and 570: Miscellaneous Exotica 549 15.2.3 Pr
Page 571 and 572: Miscellaneous Exotica 551 Most rece
Page 573 and 574: Miscellaneous Exotica 553 Fig. 15.1
Page 575 and 576: Miscellaneous Exotica 555 A violati
Page 577 and 578: Miscellaneous Exotica 557 nuclei it
Page 579 and 580: Miscellaneous Exotica 559 mass, and
Page 581 and 582: Miscellaneous Exotica 561 backgroun
Page 583 and 584: Miscellaneous Exotica 563 SN 1987A
Page 585 and 586: Miscellaneous Exotica 565 which led
Page 587: Miscellaneous Exotica 567 For a nar
Page 591 and 592: Neutrinos: The Bottom Line 571 Neut
Page 593 and 594: Neutrinos: The Bottom Line 573 Apar
Page 595 and 596: Neutrinos: The Bottom Line 575 is d
Page 597 and 598: Neutrinos: The Bottom Line 577 of t
Page 599 and 600: Neutrinos: The Bottom Line 579 siti
Page 601 and 602: Units and Dimensions 581 In the ast
Page 603 and 604: Appendix B Neutrino Coupling Consta
Page 605 and 606: Appendix C Numerical Neutrino Energ
Page 607 and 608: Numerical Neutrino Energy-Loss Rate
Page 609 and 610: Numerical Neutrino Energy-Loss Rate
Page 611 and 612: Appendix D Characteristics of Stell
Page 613 and 614: Characteristics of Stellar Plasmas
Page 627 and 628: References 607 Akhmedov, E. Kh., an
Page 629 and 630: References 609 Bahcall, J. N., Kras
Page 631 and 632: References 611 Bilenky, S. M., and
Page 633 and 634: References 613 Cannon, R. D. 1970,
Page 635 and 636: References 615 Cooper-Sarkar, A. M.
Page 637 and 638: References 617 Dodelson, S., Friema
Page 639 and 640:
References 619 Fukuda, Y., et al. 1
Page 641 and 642:
References 621 Goyal, A., Dutta, S.
Page 643 and 644:
References 623 Hoogeveen, F., and S
Page 645 and 646:
References 625 Kawakami, H., et al.
Page 647 and 648:
References 627 Landau, L. D., and P
Page 649 and 650:
References 629 Mayle, R. W., and Wi
Page 651 and 652:
References 631 Nieves, J. F., and P
Page 653 and 654:
References 633 Pochoda, P., and Sch
Page 655 and 656:
References 635 Ross, J. E., and All
Page 657 and 658:
References 637 Shlyakhter, A. I. 19
Page 659 and 660:
References 639 Totsuka, Y. 1993, Ne
Page 661 and 662:
References 641 Wiezorek, C., et al.
Page 663 and 664:
Acronyms 643 L l.h. l.h.s. ly LMC L
Page 665 and 666:
Symbols 645 dp differential in phas
Page 667 and 668:
Symbols 647 X j Peccei-Quinn charge
Page 669 and 670:
Subject Index A α-Ori 189 A665, A1
Page 671 and 672:
Subject Index 651 Coulomb gauge 204
Page 673 and 674:
Subject Index 653 H Hayashi line 32
Page 675 and 676:
Subject Index 655 multiple scatteri
Page 677 and 678:
Subject Index 657 neutrino radiativ
Page 679 and 680:
Subject Index 659 Primakoff process
Page 681 and 682:
Subject Index 661 SN 1987A bounds (
Page 683 and 684:
Subject Index 663 supernova core bi
show all

Stars as Laboratories for Fundamental Physics - MPP Theory Group

You also want an ePaper? Increase the reach of your titles

Delete template?

Save as template?