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On Local Approximations to the Nonlinear Evolution of Large‐Scale Structure

  • Authors: Martín Makler, Takeshi Kodama, and Maurício O. Calvão

Makler, Kodama, & Calvão 2001 The Astrophysical Journal 557 88.

  • Provider: AAS Journals

Caption: Fig. 2.

(a) Collapse time as a function of the initial conditions for overdense perturbations with ﹩\delta _{0}=1﹩. The contours of constant collapse time, expressed by the scale factor ac, are displayed for the ZA. The thin (thick) contours are spaced by 0.1 (0.5) in ac, with the outermost contour being ﹩a_{c}=0.4﹩ and the central value ﹩a_{c}=3﹩. (b) Same as (a) except that the MZA is used. The innermost contour is ﹩a_{c}=1.6﹩. (c) Same as (a) except that the DTA is used. The innermost contour is ﹩a_{c}=1.6﹩. (d) Same as (a) except that the CZA is used. The innermost contour is ﹩a_{c}=1.7﹩. (e) Same as (a) except that the LTA is used. The innermost contour is ﹩a_{c}=1.6﹩. (f) Signs of ﹩\lambda ^{0}_{i}﹩ in each region of the parameter space of initial conditions, with ﹩\delta _{0}=1﹩. The inner region corresponds to the values of ﹩\lambda ^{0}_{i}﹩ that can be spanned by a homogeneous ellipsoid with any axis ratios. Spherical, planar, and cylindrically symmetric perturbations are marked with a cross, a plus sign, and an asterisk, respectively. The upper parts of these graphs, which correspond to ﹩0\leq \alpha _{0}\leq \pi ﹩, have ﹩\lambda ^{0}_{3}> \lambda ^{0}_{2}> \lambda ^{0}_{1}﹩. The lower one covers the same values of ﹩\lambda ^{0}_{i}﹩, through a permutation of the indices.

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