Linear vs non linear matter power spectrum

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The discussion focuses on the distinction between linear and non-linear matter power spectra in cosmology, particularly in relation to large-scale structure formation. The power spectrum is defined as the Fourier transform of the 2-point correlation function of the density field, applicable at both large and small scales. At large scales, linear dynamics are accurate, while non-linear gravitational collapse becomes significant at smaller scales. The conversation suggests that the non-linear power spectrum should be used where noticeable differences from the linear spectrum occur, although a precise boundary is not established. Resources like Peebles' work are recommended for further understanding of these concepts.
Jip
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Hi,

I have troubles understanding the difference between linear and non linear matter power spectrum. These words are commonly used in the litterature, but I have found no definitions yet.

My understanding is that there is one definition of the power spectrum for matter distribution, basically as the Fourier transform of the 2-point correlation function of the density field.

It covers both very large scales where linear approximation for the dynamics should be accurate, while at small scales the non linear gravitational collapse heavily impacts the dynamics.
Still, we have only one power spectrum.

So, what does linear or nonlinear power spectrum refers to? (in terms of maths, I mean)

Thanks for your help!
 
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If you graph a linear relation the graph will show a straight line whether or not its flat, diagonal or vertical. This is described as value a is directly or indirectly proportional to value b.
A non linear relation will be a curve, examples include bell curves, sinusoidal wave forms
etc. Hence non linear.
value a is exponentially proportional to b. This type of relation will give a bell curve
 
Yes, I'am aware of this, but I'm rather talking about mathematical description of large scale structure formation! I have found that details can be found in peeble's book, 1980. But I don't have it. Any other ref is welcome! :)
 
Ah ok wasn't sure on what you were unclear on. I may have an article that will help but I'll have to dig around in my archives to find it.
 
Jip said:
Hi,

I have troubles understanding the difference between linear and non linear matter power spectrum. These words are commonly used in the litterature, but I have found no definitions yet.

My understanding is that there is one definition of the power spectrum for matter distribution, basically as the Fourier transform of the 2-point correlation function of the density field.

It covers both very large scales where linear approximation for the dynamics should be accurate, while at small scales the non linear gravitational collapse heavily impacts the dynamics.
Still, we have only one power spectrum.

So, what does linear or nonlinear power spectrum refers to? (in terms of maths, I mean)

Thanks for your help!
Well, I think the general idea is to start using the non-linear power spectrum at the scales in which there is a noticeable difference between the linear power spectrum and the non-linear approximations. I doubt there is a firm limit on precisely where this occurs, but the best way to investigate it is probably to start investigating some nonlinear power spectrum approximations.
 
https://en.wikipedia.org/wiki/Recombination_(cosmology) Was a matter density right after the decoupling low enough to consider the vacuum as the actual vacuum, and not the medium through which the light propagates with the speed lower than ##({\epsilon_0\mu_0})^{-1/2}##? I'm asking this in context of the calculation of the observable universe radius, where the time integral of the inverse of the scale factor is multiplied by the constant speed of light ##c##.
Why was the Hubble constant assumed to be decreasing and slowing down (decelerating) the expansion rate of the Universe, while at the same time Dark Energy is presumably accelerating the expansion? And to thicken the plot. recent news from NASA indicates that the Hubble constant is now increasing. Can you clarify this enigma? Also., if the Hubble constant eventually decreases, why is there a lower limit to its value?
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