Stars as Laboratories for Fundamental Physics - MPP Theory Group

More documents

Recommendations

Info

64 Chapter 2 convert to an absolute bolometric brightness difference ∆M tip HB rather than using the visual brightness difference ∆VHB. tip Fig. 2.18. Evolutionary speed on the RGB for a model with M = 0.8 M ⊙ , metallicity Z = 10 −4 , and initial helium abundance Y = 0.240 (Raffelt and Weiss 1992). The dashed line is the tangent near the bright end. Fig. 2.19. Luminosity function of the RGB of the globular cluster NGC 2808 which has [Fe/H] = −1.37 (Fusi Pecci et al. 1990).
Anomalous Stellar Energy Losses Bounded by Observations 65 A very important measure of the speed of evolution of a single star along the RGB, HB, and AGB is the relative number of stars found on these branches in a given cluster. Because for these advanced evolutionary phases a single-star track is essentially an isochrone, these number ratios R give us directly the relative amounts of time spent on these branches (“R-method”). For example, a novel energy-loss mechanism that operates mostly in the nondegenerate core of an HB star would shorten the helium-burning lifetime. This possibility is constrained by the relative number of stars found on the HB and RGB where the RGB in this context refers to that part which is brighter than the HB. When a star ascends the RGB, its hydrogen-burning shell encounters at some point a discontinuity in the composition profile left behind by a previous deep penetration of the envelope convection into the region of varying hydrogen content caused by nuclear burning. The ascent is briefly interrupted and the star stays at a fixed luminosity for a brief period of time. Afterward, the hydrogen shell works itself through a constant composition profile which was prepared by the convective envelope. Therefore, at a brightness near the HB one expects to find a “bump” in the number of stars on the RGB, i.e. in the distribution ∂N/∂M bol which essentially corresponds to dt/dM bol for a single-star evolutionary track (Fig. 2.18). The bump was recently identified in a number of clusters; for a particularly beautiful example see Fig. 2.19. It has been suggested to use it as a standard candle to calibrate the RR Lyrae brightness-metallicity relation (Fusi Pecci et al. 1990). An important observable is the absolute brightness of RR Lyrae stars which are not members of globular clusters. No reason is known why these field stars for a given metallicity should be any different from those found in a cluster and so brightness determinations of nearby RR Lyrae stars provide important information about their luminosity calibration. 2.4.2 Theoretical Relations In order to test the standard stellar-evolution picture against the observables introduced in Sect. 2.4.1 they need to be related to stellar properties such as mass and chemical composition. In the past, extensive grids of stellar evolutionary sequences have been calculated and have been used to derive analytic approximations for the connection between various stellar parameters; as a canonical standard I use the evolutionary HB and RG sequences of Sweigart and Gross (1976, 1978).
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 83: Anomalous Stellar Energy Losses Bou
Page 109 and 110: Chapter 3 Particles Interacting wit
Page 111 and 112: Particles Interacting with Electron
Page 135 and 136:
Particles Interacting with Electron
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:
Page 539 and 540:
Page 541 and 542:
Page 543 and 544:
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 and 588:
Miscellaneous Exotica 567 For a nar
Page 589 and 590:
Neutrinos: The Bottom Line 569 the
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 615 and 616:
Page 617 and 618:
Page 619 and 620:
Page 621 and 622:
Page 623 and 624:
Page 625 and 626:
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

Create successful ePaper yourself

Delete template?

Save as template?