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here is a link to Friedmann equations post at PF
https://www.physicsforums.com/showthread.php?p=210120#post210120
this link should be better---dont happen to have a better at the moment tho.
I actually am not sure I understand some of your questions about the
Hubble law proportionality.
Earlier I may have spoken too quickly or sloppily and given the impression that it is not a simple proportionality.
It is really really straightforward
Lets say we solve c = H d for a distance d at which things are receding at speed of light. and say it comes out d = 14 billion LY
then at 7 billion, things are receding at 1/2 c
and at 14 billion, at c
and at 21 billion, receding at 3/2 c
and at 28 billion, receding at 2 c
and so on
this is at this moment.
the presentday Hubble parameter does not tell about the past.
to find out about the past you have to solve the Friedmann equations going back into past----this is what Ned Wright and Siobahn cosmology calculators do for you and why it is important to play with the calculators a bit---there are also animations on the web that track a(t) graphically with various assumptions about how it starts off---but I like the calculators.
the thing is, in the past a(t) was different and a'(t) was different, and
H(t) was different! So how can you expect me to talk about past just using the information that right at this moment the expansion parameter H
is 71 km/sec per Mpc? Cant do it.
Yes one can do approximations, because H(t) changes only very slowly. So if you only go back 10 million or 100 million years it might look roughly the same.
But if you want to go back 10 billion years then H(t) will be very different.
However the Ned and Siobahn calculators will tell you what it is!
Like, I often see figures like H = 200 back early because expansion was faster then. then it slowed down, now it is very gradually speeding up.
this is what differential equations do. they generate beautiful curves.
but the curves have to be calculated! so you need a calculator to track the past history of a(t)-----the past history of the expansion of the U.
maybe I can find a graphic plot of the a(t) curve and give you a link.
anyway, at anyone instant of time there is a Hubble parameter H(t) and the recession speeds are proportional to distance by this straightforward
linear proportion v = Hd.
solving for the Hubble distance is easy, put c = 3E5 kilometers/sec
and put c = H D and solve for D
so 3E5 km/s = (71 km/s per Mpc) D
So you divide 300,000 by 71 and find that D has to be like 4225 Mpc :zzz:
or 4.2 Gpc and since a Gigaparsec is 3.26 billion LY you multiply by
3.26 and get that D is around 14 billion LY.
The problem here is that
specialists habitually use awkward units and for historical reasons astronomers got the nasty habit of saying parsec----a somewhat off-putting synonym for 3.26 light years.
https://www.physicsforums.com/showthread.php?p=210120#post210120
this link should be better---dont happen to have a better at the moment tho.
I actually am not sure I understand some of your questions about the
Hubble law proportionality.
Earlier I may have spoken too quickly or sloppily and given the impression that it is not a simple proportionality.
It is really really straightforward
Lets say we solve c = H d for a distance d at which things are receding at speed of light. and say it comes out d = 14 billion LY
then at 7 billion, things are receding at 1/2 c
and at 14 billion, at c
and at 21 billion, receding at 3/2 c
and at 28 billion, receding at 2 c
and so on
this is at this moment.
the presentday Hubble parameter does not tell about the past.
to find out about the past you have to solve the Friedmann equations going back into past----this is what Ned Wright and Siobahn cosmology calculators do for you and why it is important to play with the calculators a bit---there are also animations on the web that track a(t) graphically with various assumptions about how it starts off---but I like the calculators.
the thing is, in the past a(t) was different and a'(t) was different, and
H(t) was different! So how can you expect me to talk about past just using the information that right at this moment the expansion parameter H
is 71 km/sec per Mpc? Cant do it.
Yes one can do approximations, because H(t) changes only very slowly. So if you only go back 10 million or 100 million years it might look roughly the same.
But if you want to go back 10 billion years then H(t) will be very different.
However the Ned and Siobahn calculators will tell you what it is!
Like, I often see figures like H = 200 back early because expansion was faster then. then it slowed down, now it is very gradually speeding up.
this is what differential equations do. they generate beautiful curves.
but the curves have to be calculated! so you need a calculator to track the past history of a(t)-----the past history of the expansion of the U.
maybe I can find a graphic plot of the a(t) curve and give you a link.
anyway, at anyone instant of time there is a Hubble parameter H(t) and the recession speeds are proportional to distance by this straightforward
linear proportion v = Hd.
solving for the Hubble distance is easy, put c = 3E5 kilometers/sec
and put c = H D and solve for D
so 3E5 km/s = (71 km/s per Mpc) D
So you divide 300,000 by 71 and find that D has to be like 4225 Mpc :zzz:
or 4.2 Gpc and since a Gigaparsec is 3.26 billion LY you multiply by
3.26 and get that D is around 14 billion LY.
The problem here is that
specialists habitually use awkward units and for historical reasons astronomers got the nasty habit of saying parsec----a somewhat off-putting synonym for 3.26 light years.
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