I How Can Data Constrain the Number of e-Folds During Inflation?

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Data cannot directly constrain the number of e-folds during inflation due to limitations in observational capabilities, particularly for inflation that occurred beyond the last 60 e-folds. The number of e-folds affects the spectral tilt of the power spectrum, but this relationship is model-dependent, meaning different inflation models yield varying results. Generally, theorists agree that at least 50 e-folds are necessary to meet flatness and entropy constraints, with many advocating for 60 e-folds. There is currently no established methodology to measure the number of e-folds directly. Understanding these constraints is crucial for developing a universe model that aligns with observational data.
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Is there any way to constrain with data how many e folds went on during inflation ( or during our era of inflation in the case of eternal inflation)?
 
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windy miller said:
Is there any way to constrain with data how many e folds went on during inflation ( or during our era of inflation in the case of eternal inflation)?
There's no way to collect data on inflation that occurred prior to the last 60 e-folds or so, since such length scales are outside today's cosmological horizon.
 
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Sort of. It depends upon the inflation model.

Basically, for a given inflation model, different numbers of e-folds of inflation result in different spectral tilt (that is, the power spectrum's shape is slightly altered by the number of e-folds).

However, this can't be done in general. This depends upon a very specific model of inflation. Other models, with other dynamics, will show very different numbers in terms of the number of e-folds. I'm not currently aware of any methodology to measure the number of e-folds directly.
 
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Most theorists would agree no less than 50 e-folds are necessary, many prefer 60.
 
It's not so much a matter of it being "necessary"...when you begin considering fewer than 50 efolds or so, you begin to have real problems satisfying the flatness and entropy constraints.
 
I mean necessary in the sense of modeling a universe consistent with the observational constraints you hint at.
 
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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