# Approximate LCDM Expansion in Simplified Math

If we restrict ourselves to a spatially flat LCDM universe model, the first Friedmann equation can be written in a very simple form. Marcus started several PF threads in a collaborative effort to develop this simplified approach.^{[1]} It is still a work in process, but here I summarize the main insights so far, the ones I reckon to be the most informative, yet relatively easy to comprehend.

To keep it of a manageable length, this is part 1 of 3 (or perhaps more). The more detailed mathematical derivations and formal references will be provided as an appendix at the end.

#### Part 1. The Hubble constant and Hubble Time

Arguably the most important equation of the LCDM model is the evolution of the fractional expansion rate (*H*) during the expansion of the universe. In other words, how the Hubble constant *H* has changed over time. If you know this function, many of the other LCDM parameters can be derived from it, because it fixes the expansion dynamics.

(1.1) [itex]H^2 – \frac{\Lambda c^2}{3} = \frac{8\pi G}{3} \rho [/itex]

*H* is the fractional expansion rate at the time, Λ is Einstein’s cosmological constant, *c* the speed of light (as a units conversion constant), *G* is Newton’s gravitational constant and *ρ* is the changing density of matter and radiation at the time. This density is expressed as a mass density and includes dark matter, but no ‘dark energy density’. The latter is covered by Λ on the left side of the equation.

As you can check, the right-hand side gives SI units of 1/s^{2}, which is also the units of *H*^{2} (it is the square of an instantaneous fractional growth rate).^{[2]} Since Λ represents a constant curvature, its SI units would be reciprocal area 1/m^{2} and multiplying by c^{2} again gives a 1/s^{2} quantity. Hence the two sides’ units agree.

It is convenient to replace the constant Λc^{2}/3 with the square of a constant growth rate *H*_{∞}^{2}, representing the square of the Hubble constant of the ‘infinite future’, when cosmic expansion will effectively have reduced matter density to zero. We then have an interesting left-hand side, i.e.

(1.2) [itex] H^2 – H_\infty^2 = \frac{8\pi G}{3} \rho [/itex]

The present value of *H*, labeled *H*_{0} (H-naught) is observed to cause cosmic distances to increase by 1/144% per million years. Since we are observing back into the past, we also deduced how it has changed over time. It has gradually reduced from a higher value and is predicted to settle at a constant value *H*_{∞} = 1/173% per million years in the far future.

If we restrict ourselves to the era when radiation energy density is negligible compared to matter energy density,^{[3]} we can express eq. (1.2) quite simply as:

(1.3) [itex] H^2 – H_\infty^2 = (H_0^2 – H_\infty^2)/ a^3 [/itex]

The parameter *a* is the standard scale factor of cosmic expansion, which starts at near zero and equals one at present.^{[4]} In the future it will be greater than one, possibly increasing without limit. The cubed scale factor ([itex]a^3[/itex]) represents a spatial volume scale; hence the mass density [itex]\rho[/itex] changes inversely with volume.

In the long run the universe’s expansion process will be exponential at nearly the constant fractional rate *H*_{∞} and all distances will eventually grow at about *H*_{∞} = 1/173 % per million years. Exponential expansion means that all cosmic distances will increase by a factor *e* (=2.718) every 17.3 billion years (or 17.3 Gy for short). This can be called the natural ‘e-fold time’ of our universe, since an increase by a factor *e* is called an e-folding.

The 17.3 Gy e-fold time is a time scale set by Einstein’s cosmological constant. An informal study by a group of Physics-Forums contributors suggested that the 17.3 Gy time-span could be a seen as a natural timescale for our universe. For lack of an ‘official name’, the group called it a ‘zeit’, from the German word for time (Zeit). We simply take a conventional time in Gy and divide it by 17.3 Gy to get the cosmic zeit-time. This normalizes the Hubble value *H* so that it tends to unity in the far future.

Here is a graph of the thus-normalized *H* against time in zeit.

The blue dot represents our present time, 0.8 zeit and a present Hubble constant of 1.2 zeit^{-1}. The long term value of *H* asymptotically approaches the value 1 zeit^{-1}. We have not shown the function for *H* against time yet; for now it is just for illustration purposes, because we must first complete the *H* against *a* relationship.

We can easily normalize equation (1.3) to the new (zeit) scale by dividing through by *H*_{∞} (which then obviously equals 1), to get

(1.4) [itex] H^2 – 1 = (1.2^2-1)/a^3 = 0.44/a^3[/itex]

or

The Hubble time (*T_H*) is simply the inverse of *H*:

or

Here is a graph of the two equations, *H* (red) and *R = c T_H* (blue) against the expansion factor *a*, with both curves approaching the value 1.0. *T_H* has the same numerical value as the Hubble radius *R* in the graph.

These remarkably simple equations (especially 1.5 and 1.6) form the basis of a surprisingly large number of modern cosmological calculations (at least for flat space). And what’s more, they are easy to work out on most hand-held calculators. Or one can just type them into Google (with a discrete value for *a*) and it will spew out the answer.^{[5]}

More about this in Part 2, where we will also discuss the other, arguably more interesting cosmic values that can be derived using this simplified approach.

=0=

End-notes:

[1] “From Aeon to Zeon to Zeit, simplifying the standard cosmic model” by Marcus

[2] The traditional unit of the Hubble constant as used by Edwin Hubble is kilometers per second per Megaparsec. From an educational p.o.v. it was an unfortunate choice, because it seems to imply a recession speed, while it is really a fractional rate of increase of distance. It is a distance divided by a distance, all divided by time. So its natural unit is 1/time, for which we can choose any convenient timescale, e.g. per second, per year, per million years, or whatever.

[3] The ‘radiation negligible’ approximation is pretty good from about 100 million years after the start of expansion, when the radiation energy density dropped to less than 1% of the matter energy density.

[4] The cosmological scale factor *a* = 1/(*z*+1), where *z* is the cosmological redshift, e.g. if we observe a very distant galaxy at redshift *z* = 9, the scale factor at the time when the presently observed light left the galaxy has been *a *= 1/10. Thus the wavelength of the emitted light has been ‘stretched’ by a factor *S *= 1/*a *= 10, a value also used on this forum.

[5] In order for Google to calculate the equations, it has to be entered in the form (0.443/*a*^3+1)^(0.5), where any specific value has be substituted in the place of *a*. If you use *a* = 0.1, you should get *H* = 21. Google does not know the unit ‘zeit’ or ‘zeit^{-1}‘, because it is a dimensionless number anyway – we divide time by time to arrive at it.

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Play music, Read relativity and cosmology

Great work thank you I have some question where should I post it ?

Pleasure, but as a first post in Insights, I'm still struggling with formatting the figures and graphs. When I edited the entry, things got worse, so please be patient while I'm trying to sort it.

Expansion rate is H.The observable universe radius is R.Now the expansion rate is 0.07% per billion years.And it goes 0.06% per billion year.It means R is now R+ 7R/100 is universe radius for now one billion years later it will be R+7R/100+(6(R+7R/100)/100).

Zeit is 1/17,3.Now time is 0,8 zeit(13.7 Gyr) and hubble constant 1,2 zeit[SUP]-1[/SUP] which 1,2/17.3 which its 0.07.

I didnt understand mathematical expression between H and zeit.1/H is hubble time.I know but I camt make the connection.

And how we found 0.07% ? and whats the lamda is zeit units ?

If all this true you said H is equal ##H=√(0.44/a^3+1)## a is now 1(which you said).H=√(0.44/2)=0.46 whats that.

I said Expension rate is 0.07.Is that true ?

I asked so many question.If you help I will be happy

Thanks for help

Ok,I can wait

The radius of the observable universe is not directly related to the Hubble constant H. What is directly related is the Hubble radius, because it is c/H, but you will have to wait for Part 2 for more on that.

Even the Hubble radius is not increasing at 0.07% per million years today – it is the distance to some distant galaxy that is increasing at this rate. Contemplate that and I will get back to you once I have the formatting issues cleared out.

Let me clear things up then.Lets suppose theres a galaxy 5 billion light years away.Now the universe expands 1/144% per billion year so the lenght will be 5+5.1/14.4 billion light years away.The billion later this distance will be 5+5.1/14.4+(5+5.1/14.4)/17.3 billion light years.

H[SUB]∞[/SUB]=1/173 % per billion year in the future isnt it ? So now H is 1/144 % per billion year.

0.2 zeit the expansion rate was 4 zeit[SUP]-1[/SUP] which it means 4/17.3 billion years (0.23) means when the universe is 3.46 billion years old the distance will grow 0.23 times ?

If these things are true the I dont have another question

Note for Mentors:After clarification of my questions you can delete my comments

It’s 1/144% per million years, not per billion years. In a million years your 5 Gly distance will increase to 5+5/(144*100)= 5.00347 Gly. In the following million years it will increase to 5.00347+5.00347/(144*100)= 5.000694 Gly, assuming that H will change negligibly over the next million years.

It does not accurately hold for a billion years, because H will be changing noticeably in a billion years, going down to a constant 1/173% per Gy in the very far future. But since the distances are increasing faster than what H is declining, the expansion is accelerating.

I do not know where you got these values from, but they are wrong. At T=0.2 zeit, H ~ 3.4 zeit[SUP]-1[/SUP], but it is hard read from the first graph (it was just to illustrate the zeit scale). We have not yet dealt properly with H against time, which will follow in Part 2. Part 1 is primarily about H against scale factor a.