de Sitter model

de Sitter model

(dĕ-sit -er) See cosmological models.
References in periodicals archive ?
In de Sitter model, the scale factor is taken as R = [e.sup.((m+1)/2)[xi]t], where [xi] is a positive constant.
In the de Sitter model, the dark energy density decreases with increase in time and asymptotically reduces to a positive constant.
In the de Sitter model, DE dominates at late phase of EoS parameter and bulk viscous fluid plays an important role at early universe.
In a Universe devoid of matter described by equations (4.4), the Weyl conformal trace-free tensor [C.sub.[alpha][beta][gamma][mu]] never vanishes, in contrast to the de Sitter model equipped with curvature (4.6).
The de Sitter model. We can display the intriguing model discovered in 1917 by the Dutch astronomer Willem de Sitter by running the program with any choice of [H.sub.0], [[Omega].sub.0] = 0, and [[Omega].sub.[Lambda]] = 1.
It is observed that for z = 1 (i.e., at initial time) it is infinite but at z = 0 (i.e., at present time) it is closer to zero and at z = -1 it completely dies out which matches with the present day observations, which indicate that our model at present time (z = 0) is closer to the de Sitter model and attains complete de Setter model at z = -1; i.e., we can say that the Bianchi type-I space-time reduces to flat FRW (isotropic) soon after the inflation.