Stars as Laboratories for Fundamental Physics - MPP Theory Group

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514 Chapter 13 ν e ’s are detected. These expectations are borne out by the numerical results shown in Fig. 13.6. A doubling of the number of flavors is probably excluded by the observed signal duration. 13.7 Neutrino Opacity The cooling time scale of a young SN core is determined by the neutrino opacities which in turn are dominated by the neutral-current scattering ν + N → N + ν of neutrinos on nucleons. Apart from final-state Pauli blocking effects these opacities are given in terms of the scattering cross section σ = (G 2 F/π) (CV 2 + 3CA) 2 Eν 2 where the neutral-current nucleon weak-coupling constants C V,A were given in Appendix B. Therefore, the neutrino opacities are dominated by the axial-vector, i.e. the nucleon spin-dependent interaction. In Sect. 4.6.7 it was discussed that a naive application of perturbation theory in a nuclear medium likely is not appropriate because of the large spin fluctuation rate implied by this method. It would indicate that the spin of a given nucleon fluctuates so fast in a SN core that a neutrino would “see” on average a nearly vanishing contribution. This would lead to a decrease of a typical axialvector scattering rate as estimated in Fig. 4.9. To test if such a suppression effect is compatible with the SN 1987A neutrino signal, Keil, Janka, and Raffelt (1995) calculated a series of protoneutron star cooling sequences with modified neutrino opacities. To this end they substituted CA 2 → F CA 2 in the numerical subroutine which evaluates the opacities where F = (1 − a) + a (13.12) 1 + b with b = 1 12 ( ) 2 ( Γσ ≈ T ) 2 ρ 10 MeV . (13.13) 3×10 13 g cm −3 T Here, a = 1 represents full suppression while smaller values of a allow one to dial a lesser reduction of the opacities. The predicted neutrino signal at IMB and Kamiokande II was, again, characterized by the total number of expected events N IMB and N KII as well as the signal durations t IMB and t KII which represent the time at which 90% of the total number of expected events have been accrued. In Fig. 13.7 these quantities are shown as a function of a where the suppression effect was implemented for both, neutral- and chargedcurrent axial-vector interactions. The results marked with open circles
What Have We Learned from SN 1987A 515 Fig. 13.7. Number of events in the Kamiokande and IMB detectors as well as the signal durations as a function of the assumed “opacity suppression parameter” defined by Eq. (13.12). Filled circles refer to a suppression of both neutral- and charged-current axial-vector interactions while open circles refer to a suppression of neutral-current interactions only. (Adapted from Keil, Janka, and Raffelt 1995.) refer to a suppression of the neutral-current reactions alone. The modification of the results between those cases is relatively minor, indicating that the neutral-current interactions represent the dominant opacity source for the overall cooling time scale. The increase of the counting rates at the two detectors with decreasing opacities is explained by the neutrino sphere moving to deeper and hotter layers, yielding larger neutrino energies. The detectors register mostly ν e ’s so that the number of events is relatively sensitive to the charged-current opacity which affects only the electron flavor. N IMB is particularly sensitive to the ν e spectrum because of its high threshold.
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Georg G. Raffelt Stars as Laborator
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Table of Contents Preface (xiv) Ack
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Table of Contents vii 4.5 Neutrino
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Table of Contents ix 8. Neutrino Os
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Table of Contents xi 12. Radiative
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Table of Contents xiii 16.3 New Int
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Preface xv Second, particles from d
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Preface xvii search for proton deca
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Preface xix cuts of higher-order gr
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Preface xxi quoted “astrophysical
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Chapter 1 The Energy-Loss Argument
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The Energy-Loss Argument 3 example
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The Energy-Loss Argument 5 trinos,
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The Energy-Loss Argument 7 As a sim
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The Energy-Loss Argument 9 The most
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The Energy-Loss Argument 11 against
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The Energy-Loss Argument 13 ing M;
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The Energy-Loss Argument 15 M ′ (
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The Energy-Loss Argument 17 Table 1
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The Energy-Loss Argument 19 ing to
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The Energy-Loss Argument 21 scalars
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Chapter 2 Anomalous Stellar Energy
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Anomalous Stellar Energy Losses Bou
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Chapter 3 Particles Interacting wit
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Particles Interacting with Electron
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Chapter 4 Processes in a Nuclear Me
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Processes in a Nuclear Medium 119 t
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Processes in a Nuclear Medium 121 f
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Processes in a Nuclear Medium 123 F
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Processes in a Nuclear Medium 129 v
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Processes in a Nuclear Medium 131 4
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Processes in a Nuclear Medium 133 i
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Processes in a Nuclear Medium 135 H
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Processes in a Nuclear Medium 137 I
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Processes in a Nuclear Medium 143 i
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Processes in a Nuclear Medium 145 s
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Processes in a Nuclear Medium 147 E
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Processes in a Nuclear Medium 149 a
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Processes in a Nuclear Medium 151 T
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Processes in a Nuclear Medium 153 r
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Processes in a Nuclear Medium 155 4
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Processes in a Nuclear Medium 157 I
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Processes in a Nuclear Medium 159 t
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Processes in a Nuclear Medium 161 A
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Processes in a Nuclear Medium 163 R
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Chapter 5 Two-Photon Coupling of Lo
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Two-Photon Coupling of Low-Mass Bos
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Chapter 6 Particle Dispersion and D
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Particle Dispersion and Decays in M
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Chapter 7 Nonstandard Neutrinos The
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Nonstandard Neutrinos 253 (“spont
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Nonstandard Neutrinos 255 kinematic
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Nonstandard Neutrinos 257 95% CL ma
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Nonstandard Neutrinos 259 Fig. 7.2.
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Nonstandard Neutrinos 261 In three-
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Nonstandard Neutrinos 263 Flavor mi
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Nonstandard Neutrinos 267 The quant
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Nonstandard Neutrinos 269 dipole mo
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Nonstandard Neutrinos 271 component
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Nonstandard Neutrinos 275 moments.
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Nonstandard Neutrinos 277 7.5.2 Spi
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Nonstandard Neutrinos 279 where m
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Neutrino Oscillations 281 and hence
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Neutrino Oscillations 283 As usual
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Neutrino Oscillations 285 two-flavo
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Neutrino Oscillations 287 Fig. 8.2.
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Neutrino Oscillations 289 8.2.4 Exp
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Neutrino Oscillations 293 Apparentl
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Neutrino Oscillations 297 when the
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Neutrino Oscillations 299 If the ne
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Neutrino Oscillations 301 8.3.5 The
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Neutrino Oscillations 303 It is als
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Neutrino Oscillations 305 system, h
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Neutrino Oscillations 307 say, betw
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Neutrino Oscillations 309 1991). Th
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Oscillations of Trapped Neutrinos 3
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Chapter 10 Solar Neutrinos The curr
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Solar Neutrinos 343 Fig. 10.1. Sola
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Solar Neutrinos 345 There exist vas
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Solar Neutrinos 347 10.2 Calculated
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Solar Neutrinos 349 Fig. 10.3. Norm
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Solar Neutrinos 351 a certain range
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Solar Neutrinos 353 While helium an
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Solar Neutrinos 355 Bahcall and Pin
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Solar Neutrinos 357 Xu et al. (1994
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Solar Neutrinos 359 Table 10.4. Spe
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Solar Neutrinos 361 Table 10.5. Pre
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Solar Neutrinos 363 rates attribute
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Solar Neutrinos 365 10.3.4 Water Ch
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Solar Neutrinos 367 Fig. 10.10. Dif
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Solar Neutrinos 369 Fig. 10.13. Mea
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Solar Neutrinos 371 Table 10.9. Cur
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Solar Neutrinos 373 of order the an
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Solar Neutrinos 375 Fig. 10.16. 37
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Solar Neutrinos 377 GALLEX, or Home
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Solar Neutrinos 379 Table 10.10. Me
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Solar Neutrinos 381 deficits in all
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Solar Neutrinos 383 The ν e surviv
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Solar Neutrinos 385 The allowed ran
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Solar Neutrinos 387 10.7 Spin and S
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Solar Neutrinos 389 10.8 Neutrino D
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Solar Neutrinos 391 The small- and
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Solar Neutrinos 393 flux above its
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Chapter 11 Supernova Neutrinos The
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Supernova Neutrinos 397 Fig. 11.1.
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Supernova Neutrinos 399 beyond the
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Supernova Neutrinos 401 ate neutrin
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Supernova Neutrinos 403 Convection
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Supernova Neutrinos 405 Hayes, and
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Supernova Neutrinos 407 11.2 Predic
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Supernova Neutrinos 409 must then b
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Supernova Neutrinos 411 Figure 11.6
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Supernova Neutrinos 413 signal (Sec
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Supernova Neutrinos 415 time) on 23
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Supernova Neutrinos 417 All of the
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Supernova Neutrinos 419 to multiple
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Supernova Neutrinos 421 the final-s
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Supernova Neutrinos 423 ter of 53 e
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Supernova Neutrinos 425 Given these
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Supernova Neutrinos 427 thorough st
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Supernova Neutrinos 429 The forward
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Supernova Neutrinos 431 Another int
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Supernova Neutrinos 433 ber of ν e
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Supernova Neutrinos 435 A “normal
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Supernova Neutrinos 437 Fig. 11.19.
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Supernova Neutrinos 439 The approxi
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Supernova Neutrinos 441 be taken to
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Supernova Neutrinos 443 sense that
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Supernova Neutrinos 445 presence of
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Supernova Neutrinos 447 An even mor
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Chapter 12 Radiative Particle Decay
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Radiative Particle Decays 451 one c
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Radiative Particle Decays 453 corre
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Radiative Particle Decays 455 is no
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Radiative Particle Decays 457 Fig.
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Radiative Particle Decays 459 Fig.
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Radiative Particle Decays 461 12.3.
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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.
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Page 555 and 556: Axions 535 otic heavy quarks: only
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Page 561 and 562: Axions 541 Fig. 14.5. Astrophysical
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Page 567 and 568: Miscellaneous Exotica 547 Table 15.
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Page 573 and 574: Miscellaneous Exotica 553 Fig. 15.1
Page 575 and 576: Miscellaneous Exotica 555 A violati
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Page 579 and 580: Miscellaneous Exotica 559 mass, and
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Miscellaneous Exotica 565 which led
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Miscellaneous Exotica 567 For a nar
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Neutrinos: The Bottom Line 569 the
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Neutrinos: The Bottom Line 571 Neut
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Neutrinos: The Bottom Line 573 Apar
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Neutrinos: The Bottom Line 575 is d
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Neutrinos: The Bottom Line 577 of t
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Neutrinos: The Bottom Line 579 siti
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Units and Dimensions 581 In the ast
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Appendix B Neutrino Coupling Consta
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Appendix C Numerical Neutrino Energ
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Numerical Neutrino Energy-Loss Rate
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Numerical Neutrino Energy-Loss Rate
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Appendix D Characteristics of Stell
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Characteristics of Stellar Plasmas
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References 607 Akhmedov, E. Kh., an
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References 609 Bahcall, J. N., Kras
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References 611 Bilenky, S. M., and
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References 613 Cannon, R. D. 1970,
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References 615 Cooper-Sarkar, A. M.
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References 617 Dodelson, S., Friema
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References 619 Fukuda, Y., et al. 1
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References 621 Goyal, A., Dutta, S.
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References 623 Hoogeveen, F., and S
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References 625 Kawakami, H., et al.
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References 627 Landau, L. D., and P
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References 629 Mayle, R. W., and Wi
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References 631 Nieves, J. F., and P
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References 633 Pochoda, P., and Sch
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References 635 Ross, J. E., and All
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References 637 Shlyakhter, A. I. 19
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References 639 Totsuka, Y. 1993, Ne
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References 641 Wiezorek, C., et al.
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Acronyms 643 L l.h. l.h.s. ly LMC L
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Symbols 645 dp differential in phas
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Symbols 647 X j Peccei-Quinn charge
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Subject Index A α-Ori 189 A665, A1
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Subject Index 651 Coulomb gauge 204
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Subject Index 653 H Hayashi line 32
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Subject Index 655 multiple scatteri
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Subject Index 657 neutrino radiativ
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Subject Index 659 Primakoff process
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Subject Index 661 SN 1987A bounds (
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Subject Index 663 supernova core bi
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