Fourier transform of the density fluctuation

Click For Summary
SUMMARY

The discussion centers on the application of the Fourier transform to the equation governing density fluctuations in cosmology, specifically the equation ##\ddot{\delta} + 2H\dot{\delta} -\frac{3}{2} \Omega_m H^2 \delta = 0##. The Fourier transform is expressed as ##\delta_{\vec{k}} = \frac{1}{V} \int \delta(\vec{r}) e^{i \vec{k} \cdot \vec{r}} d^3 r##, leading to a transformed equation for ##\delta_{\vec{k}}##. The participant notes that the solution to this equation is a Gaussian function, indicating a specific type of behavior for density fluctuations in cosmological models. The textbook referenced is "Introduction to Cosmology, Second Edition" by Barbara Ryden, specifically pages 215-219.

PREREQUISITES
  • Understanding of Fourier transforms in physics
  • Familiarity with cosmological parameters such as Hubble parameter (H) and matter density parameter (Ωm)
  • Knowledge of differential equations and their solutions
  • Basic concepts of density fluctuations in cosmology
NEXT STEPS
  • Study the properties of Gaussian functions in the context of Fourier transforms
  • Explore the implications of density fluctuations on cosmic structure formation
  • Learn about the role of the Hubble parameter in cosmological models
  • Investigate the derivation and applications of the Friedmann equations in cosmology
USEFUL FOR

Students and researchers in cosmology, physicists interested in the mathematical modeling of density fluctuations, and anyone studying the dynamics of the universe's expansion.

happyparticle
Messages
490
Reaction score
24
TL;DR
Computing the Fourier transform of the density fluctuation.
There is a Fourier transform that I don't really understand in my textbook.

I have the following equation:
##\ddot{\delta} + 2H\dot{\delta} -\frac{3}{2} \Omega_m H^2 \delta = 0##

Then using the Fourier transform:
##\delta_{\vec{k}} = \frac{1}{V} \int \delta(\vec{r}) e^{i \vec{k} \cdot \vec{r}} d^3 r##

Where ##\delta(\vec{r})## is the density fluctuation.

We get
##\ddot{\delta_{\vec{k}}} + 2H\dot{\delta_{\vec{k}}} -\frac{3}{2} \Omega_m H^2 \delta_{\vec{k}} = 0##


The only function that does that is a gaussian function, I guess. I don't understand the process here.

Thank you
 
Space news on Phys.org
PeterDonis said:
Which textbook?
Introduction to Cosmology second edition by Barbara Ryden (p.215-219)
 

Similar threads

  • · Replies 4 ·
Replies
4
Views
2K
  • · Replies 10 ·
Replies
10
Views
2K
  • · Replies 3 ·
Replies
3
Views
2K
  • · Replies 1 ·
Replies
1
Views
2K
  • · Replies 12 ·
Replies
12
Views
3K
  • · Replies 2 ·
Replies
2
Views
2K
  • · Replies 9 ·
Replies
9
Views
2K
  • · Replies 1 ·
Replies
1
Views
3K
  • · Replies 5 ·
Replies
5
Views
3K
  • · Replies 10 ·
Replies
10
Views
654