) G. Efstathiou, W.J. Sutherland and S.J. Maddox, Nature 348 (1990), 705. Home/Search Document Not in Database Summary Related Articles Check |
This paper is cited in the following contexts:
Lorentz Invariance and the Cosmological Constant - Bertolami (1997) (Correct)
.... Indeed, a non vanishing cosmological constant contributing to the density parameter, by Omega 0 = 0:8 (together with Omega CDM 0 = 0:15 and Omega Baryons 0 = 0:05) allows for the power spectrum of the Cold Dark Matter (CDM) model to be consistent with both COBE and IRAS observations [34] and also to make the age of the Universe compatible with the age of the oldest globular clusters t 0 = 15:8 Sigma 2:1) Gyr [35] for 0:58 h 0 0:76 3 . Furthermore, a non vanishing upper bound for the cosmological constant also arises from gravitational lensing studies, Omega 0 0:75 ....
G. Efstathiou, W.J. Sutherland and S.J. Maddox, Nature 348 (1990) 705.
Astrophysical and Cosmological Constraints on a.. - Orfeu Bertolami (Correct)
....0 was considered in Ref. 6] seems to be unjustified since, as explained above, Omega phys 0 = 1. Moreover, as shown in Refs. 6] and [7] the power spectrum resulting from these considerations is similar to that of a low density Cold Dark Matter model with a large cosmological constant [15] which in terms of the density matter: Omega CDM 0 = 0:15 Omega 0 = 0:80 Omega Baryons 0 = 0:05 : 5) Another popular, although rather ad hoc, possibility to account for the large scale structure of the Universe consists of a mixture of Cold and Hot Dark Matter [16] Omega CDM 0 = 0:65 ....
G. Efstathiou, W. J. Sutherland and S. J. Maddox, Nature 348 (1990) 705.
Mixed Dark Matter And The Fate Of Baryon And Lepton Symmetries - Masiero Istituto (Correct)
....either the initial fluctuation spectrum or the composition of DM. To disfavour the formation of structures at small scales one could try to increase the above value of EQ . Late decaying particles [6] or a conspicuous contribution of the cosmological constant to Omega (with Omega CDM 0:2) [7] can yield such an increase of EQ . The other option to solve the problem is obvious from our previous analysis of the virtues and faults of HDM and CDM scenarios. Since they suffer from opposite problems when dealing with the structure formation, one might expect that a convenient admixture of ....
G. Efstathiou, W.J. Sutherland and S.J. Maddox, Nature 348 (1990) 705.
Mixed Dark Matter And The Fate Of Baryon And Lepton Symmetries - Masiero Istituto (Correct)
....CDM 90 Gamma 95 , Omega B 5 Gamma 10 and Omega ;fl 1 . The seed fluctuations were generated during inflation and with a scale invariant spectrum. In this model EQ 30( Omega h 2 0 ) Gamma1 Mpc. Although some problems were present even before the advent of the COBE data [3] , the situation has become rather difficult for the pure CDM scenario after COBE. With the normalization fixed at the COBE data [4] the CDM model predicts more power at small scales than observed [5] Several remedies have been proposed modifying either the initial fluctuation spectrum or ....
G. Efstathiou, W.J. Sutherland and S.J. Maddox, Nature 348 (1990) 705.
Takahiro T. - Nakamura And Yasushi (Correct)
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) G. Efstathiou, W.J. Sutherland and S.J. Maddox, Nature 348 (1990), 705.
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