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3
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84931528026
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For a recent review of the CP problem and the Peccei-Quinn mechanism, see H.-Y. Cheng, Phys. Rep. (to be published).
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6
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84931528024
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R. D. Peccei, in Grand Unified Theories and Related Topics, proceedings of the Fourth Kyoto Summer Institute, Kyoto, Japan, 1981, edited by M. Konuma and T. Maskawa (World Scientific, Singapore, 1981).
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13
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33744770736
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For general properties of invisible-axion models and for references to the original literature, see
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(1985)
Nucl. Phys.
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Kaplan, D.B.1
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20
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33750638035
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This bound, however, has a very peculiar status as emphasized by, : If inflation occurs in the early Universe and if reheating remains below vPQ, this bound depends on the assumption that the initial value of the axion field is of order vPQ. If no inflation occurs or if Treheat>vPQ, the formation and subsequent decay of axionic strings would produce many axions, and then, according to Davis, vPQ
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(1986)
Phys. Lett. B
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Davis, R.L.1
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26
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84931545604
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This model is usually referred to as the DFS model after, Ph, 104B, 199 (1981), but it was first proposed by
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(1980)
Yad. Fiz.
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Dine, M.1
Fischler, W.2
Srednicki, M.3
Lett4
Zhitnitsky, A.R.5
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27
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0000802508
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Following Cheng (Ref. 1) we propose the term ``DFSZ model.'' For an overview, see Cheng (Ref. 1) and Ref. 6.
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(1980)
Sov. J. Nucl. Phys.
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30
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84931527999
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See also Ref. 6.
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33
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0000564879
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hereafter denoted as paper II. In this work detailed references to previous studies of the question of axion emission from stellar bodies are given.
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(1986)
Phys. Rev. D
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Raffelt, G.G.1
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34
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8144228640
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where only the coherent axion production mechanism has been considered. It was then shown by M. S. Turner, Report No. Fermilab-Pub-86/150-A, 1986 (unpublished), that the Primakoff production would dominate in the relevant parameter range so that the number of relic axions is larger than originally thought. Both groups of authors have neglected axion production through decay of axionic strings (see Ref. 7). We find, however, that even then, Primakoff production remains the dominant mechanism in the range ma>wig1 eV, taking R=1. Therefore, Turner's results are quite independent of specific assumptions concerning the very early Universe.
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(1987)
Phys. Rev. Lett.
, vol.58
, pp. 171
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Kephart, T.W.1
Weiler, T.J.2
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37
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84931528000
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For a comment on this work see Ref. 41.
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38
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84931528003
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S. Tsuruta and K. Nomoto, Observational Cosmology, proceedings of the IAU Symposium No. 24, Beijing, 1986 (to be published); S. Tsuruta (private communication).
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51
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84931528001
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(unpublished). For the opposite conclusion, see D. O. Caldwell, R. M. Eisberg, D. M. Grumm, and M. S. Witherell, report, 1987 (unpublished).
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(1987)
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Avignone, F.T.1
Brodzinski, R.L.2
Miley, H.S.3
Reeves, J.H.4
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0002542349
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Nuovo Cimento 9C, 17 (1986)
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(1986)
Nuovo Cimento
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59
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84931528007
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Zh. Eksp. Teor. Fiz. 91, 7 (1986)
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64
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84931528008
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M. Cassé, S. Cahen, and C. Doom, in Neutrinos and the Present-Day Universe, edited by Th. Montmerie and M. Spiro (Editions Frontie`res, Saclay, Gif-sur-Yvette, 1986).
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68
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35949021042
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For a brief discussion of some aspects of stimulation effects in the context of stellar axion emission, see
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(1986)
Phys. Rev. D
, vol.34
, pp. 3927
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Raffelt, G.G.1
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70
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0000946833
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Stellar Evolution.VI. Evolution from the Main Sequence to the Red-Giant Branch for Stars of Mass 1 M_{sun}, 1.25 M_{sun}, and 1.5 M_{sun}
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(1967)
The Astrophysical Journal
, vol.147
, pp. 624
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Iben, I.1
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82
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84931528335
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This work, unfortunately, overestimates the axion effect, see Ref. 21.
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