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Volumn 55, Issue 4, 1997, Pages 1851-1859

Dynamical [Formula presented] models of structure formation

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Indexed keywords


EID: 0000440905     PISSN: 15507998     EISSN: 15502368     Source Type: Journal    
DOI: 10.1103/PhysRevD.55.1851     Document Type: Article
Times cited : (264)

References (51)
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    • A. Einstein, Sitzungsber. Preuss. Akad. Wiss. 1917, 142 (1917). This article is translated into English in J. Bernstein and G. Feinberg, Cosmological Constants (Columbia University, New York, 1986)
    • A. Einstein, Sitzungsber. Preuss. Akad. Wiss. 1917, 142 (1917). This article is translated into English in J. Bernstein and G. Feinberg, Cosmological Constants (Columbia University, New York, 1986).
  • 13
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    • Strictly speaking, “standard” CDM usually refers to the parameter choice (Formula presented) and (Formula presented); while such a model yields a better shape for (Formula presented) than does an (Formula presented) model with (Formula presented), the fit to the data is still poor
    • Strictly speaking, “standard” CDM usually refers to the parameter choice (Formula presented) and (Formula presented); while such a model yields a better shape for (Formula presented) than does an (Formula presented) model with (Formula presented), the fit to the data is still poor.
  • 15
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    • E. L. Wright et al., 464, L21 (1996);
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    • G. Hinshaw et al., 464, L17 (1996) for analyses of the four-year COBE data.
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    • D. Maoz and H.-W. Rix, 416, 425 (1993).
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    • G. Kauffmann, A. Nusser, and M. Steinmetz, Report No. astro-ph/9512009 (unpublished)
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    • Mo, H.J.1    White, S.D.M.2
  • 26
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    • Another fix for the amplitude problem is to introduce a small tilt to the primordial power spectrum, (Formula presented), with (Formula presented). In the models of Fig. 11, we have assumed a scale-invariant primordial spectrum with (Formula presented), but inflationary models typically predict small deviations from this, with (Formula presented) less than unity in models with a single scalar field; see, e.g
    • Another fix for the amplitude problem is to introduce a small tilt to the primordial power spectrum, (Formula presented), with (Formula presented). In the models of Fig. 11, we have assumed a scale-invariant primordial spectrum with (Formula presented), but inflationary models typically predict small deviations from this, with (Formula presented) less than unity in models with a single scalar field; see, e.g.
  • 27
    • 0001702814 scopus 로고
    • Tilted spectra in (Formula presented) models have been examined in A. R. Liddle et al., Mon. Not. R. Astron. Soc. 282, 281 (1996); S. Dodelson, E. Gates, and M. S. Turner, Science 374, 69 (1996)
    • F. Adams et al., Phys. Rev. D47, 426 (1993). Tilted spectra in (Formula presented) models have been examined in A. R. Liddle et al., Mon. Not. R. Astron. Soc. 282, 281 (1996); S. Dodelson, E. Gates, and M. S. Turner, Science 374, 69 (1996).
    • (1993) Phys. Rev. D , vol.47 , pp. 426
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    • For discussions of other scalar field and phenomenological models of a time-varying vacuum energy, see, e.g., K. Freese et al., Nucl. Phys.B287, 797 (1987);
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    • Freese, K.1
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    • (1987) , vol.B287 , pp. 776
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    • The constraints from Type Ia supernova observations are also different in these models from conventional (Formula presented) models; J. Frieman and I. Waga (in preparation)
    • The constraints from Type Ia supernova observations are also different in these models from conventional (Formula presented) models; J. Frieman and I. Waga (in preparation).
  • 38
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    • J. Bartlett et al., Science267, 980 (1995). A less extreme proposal was put forth by
    • (1995) Science , vol.267 , pp. 980
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    • Phys. Lett. B203, 125 (1988).
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    • J. A. Peacock and S. J. Dodds, Report No. astro-ph/9603031, 1996 (unpublished). See also
    • J. A. Peacock and S. J. Dodds, Report No. astro-ph/9603031, 1996 (unpublished). See also
  • 51
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    • G. Efstathiou in Physics of the Early Universe, edited by J. A. Peacock, A. F. Heavens, and A. T. Davies (Edinburgh University Press, Edinburgh, England, 1990)
    • G. Efstathiou in Physics of the Early Universe, edited by J. A. Peacock, A. F. Heavens, and A. T. Davies (Edinburgh University Press, Edinburgh, England, 1990).


* 이 정보는 Elsevier사의 SCOPUS DB에서 KISTI가 분석하여 추출한 것입니다.