Universe expansion -> t = - inifinite

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Discussion Overview

The discussion revolves around the expansion of the universe, particularly focusing on the implications of time as it relates to the universe's beginning and future. Participants explore various cosmological models, the nature of the universe's expansion, and the mathematical representations of these concepts.

Discussion Character

  • Exploratory
  • Debate/contested
  • Mathematical reasoning
  • Conceptual clarification

Main Points Raised

  • One participant suggests that considering time as negative infinity could represent the beginning of the universe, proposing limits for the diameter of the universe at different times.
  • Another participant challenges the assumption that the universe has always been expanding at an increasing rate, referencing the LambdaCDM model and suggesting that there may have been a contraction phase before the Big Bang.
  • Questions are raised about the nature of the function representing the universe's diameter over time, including whether it is always increasing or has variations.
  • One participant expresses uncertainty about the exact nature of the universe's expansion and its implications.
  • A later reply emphasizes the importance of terminology, suggesting that "scale parameter" is a more accurate term than "diameter of the universe," and discusses the implications of running time backwards in cosmological models.
  • A participant expresses a desire for simpler explanations and questions which cosmological model has more supporting evidence, specifically comparing the FRW model and the de Sitter lambdavacuum.
  • There is a query about the role of dark matter in the universe's acceleration and how this relates to the FRW model's predictions of a potential Big Crunch.

Areas of Agreement / Disagreement

Participants exhibit disagreement regarding the nature of the universe's expansion and the validity of different cosmological models. There is no consensus on which model is more justified or how to interpret the implications of current observations.

Contextual Notes

Participants acknowledge limitations in their understanding and the complexity of the models discussed. There is a recognition that some concepts may not be fully accessible to all participants, particularly those with less advanced knowledge in the field.

Who May Find This Useful

This discussion may be of interest to students and enthusiasts of cosmology, particularly those exploring the dynamics of the universe's expansion and the theoretical frameworks that describe it.

JPC
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hey

Was thinking
since the universe is actually expanding at an increasing speed
We can ask the question : how did all the matter+energy get reunite in one small point ?

well, can we just say that if we consider , 't' : time :
t=-infinite : the beginning of everything
t = 0 : today
t = +oo : the end of everything.

That if 'd' the diameter of the universe at a time t

Lim -oo (d) = 0
lim +oo (d) = +oo

Meaning, that its all about limits
 
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JPC said:
since the universe is actually expanding at an increasing speed

according to the standard (LambdaCDM) model that cosmologists mostly use, the universe has NOT ALWAYS been accelerating its expansion

for a long time (billions of years) the expansion was slowing down and the Hubble rate was decreasing

so what you see now does not tell you that it has always been doing that
=======================

a lot of work going on now is about models that have not always been expanding.

in these models there is a before-the-big-bang contraction phase and an abrupt turnaround when a critical density was reached (near the socalled Planck density)

It wouldn't have been actually a "point" as people used to imagine, but just very concentrated

If you want links to the technical papers, just say.
========================

the point is that just because at present it is doing such-and-such doesn't mean we can extrapolate back assuming that it has always

it's better to use a computer model with some quantum law of gravity built in, and actually run it backwards and see what happens-------or to use a equation model with solvable equations
either way you may find that there is a turnaround (gravity acting different at very high density)
 
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but if D = F(t)
where D : diameter of the universe (aprox)
t : time

what are the variations of the function f ?
- always increasing, (with or without constant at some intervals) : (french : croissant) ?
- Increasing, then decreasing ?
- other ?

and what are the limits of f(x) at :
- infinite and + infinite ?
 
No one really knows exactly ?
 
Shouldn't this be in the Cosmology forum?

I think you have misunderstood careless references to "diameter of the universe", which doesn't mean what (almost certainly) you think: a more correct term is scale parameter.

Of course the time dependence of the scale parameter in the FRW lambdadusts is known (as a function of proper time as measured by the dust particles). See the last chapter of the excellent undergraduate textbook by D'Inverno for the answers you seek. You can look for old sci.physic.* posts by myself discussing in detail FRW dusts with nonzero Lambda. In some cases this parameter is most conveniently expressed parametrically but in the case of flat hyperslices it can be easily written as an explicit function of "time".

More important: if you "run time backwards" in the FRW models you come to an initial time, which we call the Big Bang. (In some special cases the same thing happens if you run time forwards, except we call that the Big Crunch.) There are some other cosmological models, such as the de Sitter lambdavacuum, in which one can "run time backwards" indefinitely. It is possible to analyse the global structure of cosmological models such as FRW models and de Sitter lambdavacuum using methods pioneered by Penrose and others. See for example Hawking and Ellis, The Large Scale Structure of Space-Time, Cambridge University Press, 1973.
 
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Oh, yes maybe this post should be put in cosmology, but now that its posted the forum won't let me change its location.

Thanks for all the references you have given me, but I am just a 12th grade student in a French semi-International Scientific section, i don't want to get lost in High level explanations until i reach the scientific level.

Im just looking for simple explanations for a general understanding. I will be looking for the details latter in my post-school studies.

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but which model as more proof, justification :
- FRW or de Sitter lambdavacuum ?

Right now the universe is expanding at an increased rate.
Is it because of black matter with a negative mass that acts as a expansion force ?

And if the Universe is accelerating, how does FRW explain that the universe will come back together in a big crush ?
 

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