17. Beginning inflation: problem of initial conditions in cosmology (Inflationary perturbations 4)

Posted by Dmitry
April 11, 2008

This is the next post in the series based on my lectures on inflationary perturbations and large scale structure given at the University of Helsinki. Today we will finally start to discuss the physics of inflation.

To get a theoretical prediction for the correlation functions of \delta at observable scales as well as their dependence on the redshift z, it is not enough to know the general solution of equations governing the dynamics of cosmological perturbations; one also has to know the initial conditions for them - namely, the distribution of matter at some moment of time in the early Universe as well as the distribution of velocities of the matter particles. Initial conditions should be defined at a time scale not earler than the Planckian time t_{P}\sim10^{-44} sec, since quantum corrections to GR become important at t\sim t_{P}. From the observations we are able to conclude that the initial distributions of matter density and velocity field had very special, in a sense unnatural forms. What was so unnatural about them?

As we know, the Universe at scales larger than a hundred of MPcs is extremely homogeneous - namely, the average amplitude of the density fluctuation \delta\rho/\rho_{0} is of the order of 10^{-5}. Since large scales correspond to earlier moments of time in the history of the Universe, the distribution of matter in the early Universe was homogeneous to the same extremely fine-tuned degree as well. To understand how exactly large is the fine-tuning, let us do a quick estimation.

The current size of homogeneous isotropic region in the Universe is at least of the same order as the horizon scale

l_{H}\sim ct_{0}\sim13\,{\rm Glyrs}\sim10^{28}\,{\rm cm},

where t_{0} is the age of the Universe. Since any physical length in the expanding universe grows as a, in the very beginning of the evolution of the Universe the homogeneity scale was much lower:

l_{i}\sim ct_{0}\frac{a_{i}}{a_{0}}=ct_{0}\frac{T_{0}}{T_{i}}

(we took into account the fact the temperature T drops as T\sim a^{-1} in the expanding universe and used notation a_{0} for the present value of scale factor). If we suppose that the temperature of primordial plasma was T_{i}\sim T_{P}\sim10^{32}\,{\rm K} at the Planckian time, we find that \frac{a_{i}}{a_{0}}\sim10^{-32}, so the initial size of the homogeneous patch in the Universe was of the order of 10^{28}\, l_{P}, where l_{P}=ct_{P} is the Planckian length scale determining the size of the causal patch at the Planckian time.

Naively, it is impossible to have strong correlations in the matter distribution at scales larger than the size of a causally connected region; however, it looks like that in the beginning of its evolution the Universe consisted of (10^{28})^{3}=10^{84} causally disconnected regions, and the matter distribution was highly correlated between them - indeed, it was homogeneous everywhere in the region with the size l_{P}. Estimating \dot{a}=aH\sim\frac{a}{t}, we find

\frac{l_{i}}{l_{P}}\sim\frac{\dot{a}_{0}}{\dot{a}_{i}}\sim10^{-28}.

Thus, it looks like the ratio \frac{\dot{a}_{0}}{\dot{a}_{i}} is incredibly fine-tuned. What we have just described is the essence of horizon and homogeneity problems of the standard Big Bang cosmology.

Similar issues to be explained are why the present Universe is extremely isotropic at horizon scale l_{H} and why it was so close to be absolutely spatially flat in the beginning of its evolution. Let us discuss the second issue a bit more. The question can be reformulated as follows: why the average energy density in the Univere is so extremely close to the critical value

\Omega=\frac{\rho}{\rho_{{\rm critical}}}\sim1?

Rewriting the Friedmann equation as

\Omega(t)-1=\frac{k}{(Ha)^{2}},

where k is the spatial flatness parameter, we see that

\Omega_{i}-1=(\Omega_{0}-1)\frac{(H_{0}a_{0})^{2}}{(H_{i}a_{i})^{2}}=
=(\Omega_{0}-1)\left(\frac{\dot{a}_{0}}{\dot{a}_{i}}\right)^{2}\lesssim10^{-56}

in the early Universe. Why the spatial flatness of the early Universe was so extremely fine-tuned to be close to 0? This problem as known as the spatial flatness problem of the standard Big Bang cosmology.

Finally, we notice that the total present entropy of the observable part of the Universe is of the order of S\sim10^{87}. Why it is so huge? One has to explain this number, and the explanation should be based on the initial conditions we introduce.

  • Digg
  • StumbleUpon
  • Technorati
Cosmological perturbations and large scale structure, Cosmology, Entered Apprentice

If you enjoyed this post, please consider to leave a comment, subscribe to the RSS feed or get new posts sent directly to your Inbox. If you are interested to know what I am doing right now, follow me on Twitter. The posts below are probably related to the subject of this one:

Best posts
24. Inflation: description in terms of hydrodynamics (Inflationary perturbations 4)
53. Eternal inflation: stochastic approach 1 (Inflationary perturbations 7)
111. Talk in Munich. One interesting infrared scale in inflationary cosmology
99. Eternal inflation with many light scalar fields

RSS feed | Trackback URI

Comments »

No comments yet.

Name
E-mail
URI
Subscribe to comments via email
Your Comment (smaller size | larger size)
You may use <a href="" title=""> <abbr title=""> <acronym title=""> <b> <blockquote cite=""> <cite> <code> <del datetime=""> <em> <i> <q cite=""> <strike> <strong> in your comment.

Trackback responses to this post