Stars as Laboratories for Fundamental Physics - MPP Theory Group

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364 Chapter 10 Table 10.6. Predicted absorption rate (in SNU) by 71 Ga for different solar source reactions. BP92 give “theoretical 3σ” uncertainties. Diffusion pp pep 7 Be 8 B 13 N 15 O Total BP95 He, metals 69.7 3.0 37.7 16.1 3.8 6.3 137 +8 −7 BP92 He 70.8 3.1 35.8 13.8 3.0 4.9 131.5 +21 −17 BP92 — 71.3 3.1 32.9 12.3 2.7 4.3 127 +19 −16 TL93 — 71.1 3.0 30.9 10.8 2.4 3.7 122.5 ± 7 BP92 = Bahcall and Pinsonneault (1992). BP95 = Bahcall and Pinsonneault (1995). TL93 = Turck-Chièze and Lopes (1993). The GALLEX experiment was subjected to an “on-off test” by virtue of a laboratory ν e source strong enough to “outshine” the Sun in its local neutrino flux (GALLEX collaboration 1995a). To this end a container with activated chromium was inserted in the center of the tank containing the target fluid. The relevant isotope is 51 Cr which decays to 51 V with a half-life of 27.71 d by electron capture. The ν e spectrum consists of four monoenergetic lines of energies 426 keV (9%), 431 keV (1%), 746 keV (81%), and 751 keV (9%). The dominating line is very close to the solar beryllium line. An analysis of the first seven exposures reveals a ratio between the measured and expected counting rate of 1.04 ± 0.12. At the present time, four further extractions are still being analyzed. Meanwhile, the source is being reactivated at the Siloé nuclear reactor in Grenoble (France) in order to perform further exposures. The GALLEX collaboration has interpreted the source experiment as a global test of their detector efficiency. Most recently, Hata and Haxton (1995) have advocated a somewhat different view. They argue that the gallium absorption cross section for the 746 keV line is poorly known because of excited-state contributions which have not been directly measured, and which are more uncertain than had been acknowledged in the previous literature. According to Hata and Haxton the source experiment should not be taken as measuring, say, the GALLEX extraction efficiency but rather as measuring the excited-state contributions to the absorption cross section for beryllium neutrinos.
Solar Neutrinos 365 10.3.4 Water Cherenkov Detector (Kamiokande) A water Cherenkov detector like the one located in the Kamioka metal mine (Gifu prefecture, Japan) is a large body of water, surrounded by photomultipliers which register the Cherenkov light emitted by relativistic charged particles. Solar neutrinos are detected by virtue of their elastic scattering on the electrons bound in the water molecules, ν + e → e + ν. (10.14) This process has no significant threshold, although in practice the detection of the electrons is background-limited to relatively large energies. The Kamiokande detector began its measurement of solar neutrinos in January 1987 with an effective analysis threshold of about 9 MeV which was reduced to about 7 MeV in mid 1988. The much larger Superkamiokande detector, which is scheduled to begin data-taking in April 1996, will have a threshold of about 5 MeV. In contrast with the radiochemical detectors which are effectively based on the charged-current reaction ν e + n → p + e, the elastic scattering on electrons is sensitive to all (left-handed) neutrinos and antineutrinos. The cross section is given by the well-known formula (e.g. Commins and Bucksbaum 1983) [ dσ νe dy = G2 Fm e E ν A + B (1 − y) 2 − C y m ] e , (10.15) 2π E ν where G F is the Fermi constant and the coefficients A, B, and C are tabulated in Tab. 10.7. Further, y ≡ E ν − E ν ′ = T e 2E ν and 0 < y < , (10.16) E ν E ν 2E ν + m e where E ν and E ν ′ are the initial- and final-state neutrino energies while T e is the kinetic energy of the final-state electron. Table 10.7. Coefficients in Eq. (10.15) for elastic neutrino electron scattering. Flavor A B C ν e (C V + C A + 2) 2 (C V − C A ) 2 (C V + 1) 2 − (C A + 1) 2 ν e (C V − C A ) 2 (C V + C A + 2) 2 (C V + 1) 2 − (C A + 1) 2 ν µ,τ (C V + C A ) 2 (C V − C A ) 2 ν µ,τ (C V − C A ) 2 (C V + C A ) 2 CV 2 − CA 2 CV 2 − CA 2 C V = − 1 2 + sin2 Θ W ≈ −0.04, C A = − 1 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
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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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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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