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- W42707624 abstract "If the primordial perturbations were adiabatic and if neutrinos are massless, all fluctuations on scales smaller than the Silk length λD=2(0.036+Ωoho 2)−1 Mpc are dissipated (here Ωo is the density parameter and ho the constant in units 100 kms −1 Mpc −1), see ref. 1. The presence of massive neutrinos increases the damping length to λDv=40 M30 −1Mpc, where M30 is the average neutrino mass in units 30 eV(2). In the first order perturbation theory, the gravitational instability manifests itself by the growth of the clustering length (i.e. the lag for which the correlation function has unit value). Therefore, it seems resonable to expect that the present mass clustering length is r ≳λD, λDv . Since for the observed galaxy two-point correlation function ro=5/ho MpC (1), this condition is violated for most plausible values of the prameters Ωo h o 2 and M30. This is the so-called clustering length problem and it has been suggested as an argument against the “pancake” scenario of galaxy formation (3) ,(4)." @default.
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- W42707624 date "1984-01-01" @default.
- W42707624 modified "2023-10-16" @default.
- W42707624 title "The Non-Linear Evolution of the Clustering Length in the “Pancake” Scenario" @default.
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- W42707624 doi "https://doi.org/10.1007/978-94-009-6412-9_86" @default.
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