Stars as Laboratories for Fundamental Physics - MPP Theory Group

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48 Chapter 2 process γ → ν e ν e which is studied in detail in Chapter 6; numerical emission rates are discussed in Appendix C. The neutrino energy-loss rate as a function of temperature is shown in Fig. C.6; for a WD the short-dashed curve (2ρ/µ e = 10 6 g cm −3 ) is most appropriate. Neutrino cooling causes a depression of the WD luminosity function at the bright end. The dashed line in Fig. 2.10 represents a numerical cooling calculation for a 0.6 M ⊙ WD which included neutrinos (Koester and Schönberner 1986); the “neutrino dip” is clearly visible. The photon decay γ → νν is a neutrino process made possible by the medium-induced photon dispersion relation and by the mediuminduced effective photon-neutrino coupling (Chapter 6). As such this process is not observable in the laboratory, although there is no doubt about its reality. Still, it is encouraging to see it so plainly in the WD luminosity function. If neutrino emission were much stronger than standard, the neutrino dip would be correspondingly deeper. Stothers (1970) used the observation of several bright WDs in the Hyades cluster to constrain the efficiency of neutrino cooling; at that time the existence and magnitude of a direct neutrino-electron interaction had not yet been experimentally established. Stothers found that an emission rate 300 times larger than standard could be conservatively excluded. Recently, Blinnikov and Dunina-Barkovskaya (1994) have studied this subject in detail. Their motivation was the possible existence of a neutrino magnetic dipole moment which would enhance the effective neutrino-photon coupling and thus the efficiency of the plasma process. For the present general discussion it is enough to think of their study as an arbitrary variation of the neutrino emissivity, even though the magnetic-moment induced plasma emission rate has a different density dependence—see Eq. (6.94) for details. For the pertinent conditions the energy-loss rate induced by the assumed dipole moment µ ν is roughly 0.06 µ 2 12 times the standard one where µ 12 ≡ µ ν /10 −12 µ B (Bohr magneton µ B ). Blinnikov and Dunina-Barkovskaya (1994) calculated the luminosity function for 0.6 M ⊙ WDs for the standard case (µ 12 = 0, dashed line in Fig. 2.11) and for a roughly 25-fold increased rate of neutrino cooling (µ 12 = 20, dotted line in Fig. 2.11). The birthrate of WDs was assumed constant and adjusted to optimize the agreement with the observations. For µ 12 = 0 they needed B = 0.62×10 −3 pc −3 Gyr −1 while for µ 12 = 20 the best fit was achieved for 0.67 in these units. Blinnikov and Dunina-Barkovskaya (1994) pointed out that a particularly sensitive observable for the neutrino dip is the temperature dis-
Anomalous Stellar Energy Losses Bounded by Observations 49 Fig. 2.11. Luminosity function for 0.6 M ⊙ WDs for two values of µ 12 (Blinnikov and Dunina-Barkovskaya 1994) compared with the observations quoted in the upper part of Tab. 2.1 (Fleming, Liebert, and Green 1986). Fig. 2.12. Relative number of 0.6 and 0.8 M ⊙ WDs in the two hot temperature bins of Tab. 2.2 as a function of the anomalous neutrino cooling implied by a magnetic dipole moment µ ν (Blinnikov and Dunina-Barkovskaya 1994). The number of WDs in the temperature range 12,000−40,000 K is normalized to unity. The shaded bands correspond to the observations (Tab. 2.2).
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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
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
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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 461 12.3.
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Radiative Particle Decays 463 emiss
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Radiative Particle Decays 465 range
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Radiative Particle Decays 469 weak
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Radiative Particle Decays 471 value
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Radiative Particle Decays 473 ignor
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Radiative Particle Decays 479 Table
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Radiative Particle Decays 481 In or
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Radiative Particle Decays 485 while
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Radiative Particle Decays 487 h 100
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Radiative Particle Decays 491 still
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Chapter 13 What Have We Learned fro
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What Have We Learned from SN 1987A
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Axions 525 Table 14.1. Particle mag
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Axions 527 or axion decay constant.
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Axions 529 The Yukawa coupling h is
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Axions 531 14.2.3 Pseudoscalar vs.
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Axions 533 Notably, the Higgs field
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Axions 535 otic heavy quarks: only
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Axions 537 Various axion models dif
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Axions 539 Bounds on the Yukawa cou
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Axions 541 Fig. 14.5. Astrophysical
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Axions 543 decay into axions. This
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Chapter 15 Miscellaneous Exotica St
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Miscellaneous Exotica 547 Table 15.
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Miscellaneous Exotica 549 15.2.3 Pr
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Miscellaneous Exotica 551 Most rece
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Miscellaneous Exotica 553 Fig. 15.1
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Miscellaneous Exotica 555 A violati
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Miscellaneous Exotica 557 nuclei it
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Miscellaneous Exotica 559 mass, and
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Miscellaneous Exotica 561 backgroun
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Miscellaneous Exotica 563 SN 1987A
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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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