A post-Newtonian Lagrangian perturbation approach to large-scale structure formation

Details A post-Newtonian Lagrangian perturbation approach to large-scale structure formation A post-Newtonian Lagrangian perturbation approach to large-scale structure formation

Jun 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999mnras.306...64t&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Volume 306, Issue 1, pp. 64-88.

Astronomy and Astrophysics

Astronomy

3

Gravitation, Instabilities, Cosmology: Theory, Large-Scale Structure Of Universe

Scientific paper

We formulate Lagrangian perturbation theory to solve the non-linear dynamics of a self-gravitating fluid within the framework of the post-Newtonian approximation in general relativity, using the (3+1) formalism. Our formulation coincides with the Newtonian Lagrangian perturbation theory developed by Buchert for scales much smaller than the horizon scale, and with the gauge-invariant linearized theory in longitudinal gauge conditions for the linear regime. These conditions are achieved by using the gauge-invariant quantities at the initial time, when the linearized theory is valid. The post-Newtonian corrections in the solution of the trajectory field of fluid elements are calculated in their explicit forms. Thus our formulation allows us to investigate the evolution of large-scale fluctuations involving relativistic corrections from the early regime, such as the decoupling time of matter and radiation, until today. As a result, we are able to show that naive Newtonian cosmology for the structure formation will be a good approximation even for perturbations with scales not only inside but also beyond the present horizon scale in longitudinal coordinates. Although the post-Newtonian corrections are small, it is shown that they have a growing transverse mode, which is not present in Newtonian theory or in the gauge-invariant linearized theory. Such post-Newtonian-order effects might produce a characteristic appearance of large-scale structure formation, for example through the observation of anisotropies in the cosmic microwave background radiation (CMB). Furthermore, because our approach has a straightforward Newtonian limit, it will also be convenient for numerical implementation based on the presently available Newtonian simulations. Our results easily allow us to perform a simple order estimation of each term in the solution, which indicates that post-Newtonian corrections cannot be neglected in the early evolution of density fluctuations, compared with Newtonian perturbation solutions.

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