Ich said:
True, but that's simply because the setup of the thought experiment is set up and analyzed in a specific coordinate system. This coordinate system is not the standard one for defining velocities, yet is is supposed to be by the authors. That's why counterintuitive results follow that only make (limited) sense in the "expanding space" picture.
Try calculating the "x"-position of a really tethered galaxy in empty spacetime. Again you will find that there is much counterintuitive behaviour of the coordinates, not of physics, and that Davis and Lineweaver fail to account for that.
How do
you define "really tethered galaxy"?
(For other readers: is a serious question. Ich is my new hero for helping me fix up my errors, and to understand an error made in a different Davis and Lineweaver paper concerning SR models of ballistic expansion in a static space. (Ref: [post=2144968]msg #71[/post] of
Why "expanding space"?) I hope that here he can do it again, or else that I can return the favour. I don't know which it will be as yet.)
Obviously, galaxies are not really tethered, and so to be precise, we would have to define what we mean by giving world lines in some co-ordinate system. The definition used in Davis and Lineweaver is explicit. They mean that "proper velocity" is zero, which means the rate of change of "proper distance" with "proper time".
Furthermore, the question is not about what happens as the tether remains fixed, but what happens when a particle is released from the hypothetical tether, and follows an unaccelerated world line thereafter. Davis and Lineweaver are explicit that the problem is about a galaxy that has been "let go" from the initial condition defined by the hypothetical tether.
Given this definition, the rest follows independently of co-ordinates. For example, in a critical density model, they state that an unaccelerated particle with a proper velocity initially equal to zero will gradually approach the observer, and pass through to the other side of the sky, where it will eventually (in the limit) come to rest against the Hubble flow.
Here's a review of the relevant co-ordinate stuff, as I see it.
(A)Proper time and proper distance co-ordinates
I find it easiest to use the co-ordinates of proper time and proper distance. This is commonly used in cosmology. For example, these are the co-ordinates used in
Ned's formulae for distances in expanding space.
In this co-ordinate system, there is an essentially arbitrary choice of a world line for a non-accelerating reference particle to define distance zero, and any other spacetime point is defined by a radial distance r, by two polar co-ordinates for direction, and by a proper time co-ordinate. With these co-ordinates, the scale factor is simply a function of proper time. Different models for the universe correspond to different functions for the scale factor.
There is also a notion of "co-moving distance", which is defined as the proper distance divided by the scale factor. Co-moving observers are ones that maintain a fixed co-moving distance. In our universe, presuming a uniform cosmological background radiation, all observers that are (locally) at rest with respect to the background radiation (as determined by redshift of the radiation being equal from all directions) are co-moving observers with each other. Our Sun is currently moving at a velocity of about 600 m/s locally wrt to the cosmological background, which is a minor complication. For cosmology, it is convenient to use cosmological background as a reference point for zero proper distance, rather than the Earth itself.
The proper distance has a simple intuitive consequence. Suppose that all of space is filled with co-moving observers, each of which holds a ruler of a fixed length, defined by a light clock. That is, the ruler measures distance by seeing how far light moves, locally, in a small fixed increment of proper time. At a previously agreed common instant of proper time, all the co-moving observers between two galaxies get a reading for their rulers. The distance measured as the sum of all the rulers at a common instant of proper time is the proper distance co-ordinate, at that point in proper time. The rulers have to be co-moving, which means that the number of fixed length rulers between two co-moving objects in an expanding space is always increasing.
(B) Recession velocities
You can get different notions of velocity when you have different notions of distance. Distance, and velocity, are numbers that depend on a co-ordinate system. I'll use a "proper velocity" as the rate of change of "proper distance" with "proper time". This is a pretty conventional definition.
You can easily give other definitions. I've deleted some remarks here about other notions as a side track. But I can give them and work with them if needed.
For a co-moving particles, the proper velocity is directly proportional to rate of change of scale factor.
(C) Defining "tether"
My understanding of "tethered galaxy" is one for which the "proper velocity" is zero. It has a world line for which the proper distance remains constant with proper time. This is explicitly what Davis and Lineweaver use.
In my opinion, they are right to do so. The "proper velocity" is a standard for talking about recession velocities in cosmology, and people who have trouble understanding the notion of expanding space might just possibly benefit from thinking about what will happen to an unaccelerated particle at some great distance if it starts from a point in time with zero "proper velocity".
If they won't benefit from this thought experiment, then the Davis and Lineweaver paper is no good to them. I, however, believe I have gained useful insights into the FRW solutions by considering the tethered galaxy problem as defined and solved by Davis and Lineweaver.
If there are actual errors in their analysis, given their explicit definitions, I'll be surprised. But I've been surprised before, with respect to some plain errors in another paper concerning an incorrectly derived SR formula.
(D) Homework
You have proposed for me a homework exercise. This worked well for me last time, and I'll try it again. It may take me a bit of time, as I am busy with other projects also.
As I understand it, your homework problem can be defined formally as finding the world line of an unaccelerated particle that initially has a proper distance "r" at a time "t", and initial proper velocity 0, in an empty universe where the scale factor is simply a(t) = H
0 t. Is that right?
For reference, I am going to assume that the local momentum of an unaccelerated particle in motion wrt to the co-moving background is inversely proportional to scale factor. This is not a violation of conservation of momentum, for the same reason cosmological redshift of photons is not a violation of conservation of energy. Indeed, the locally measured momentum of photons has precisely this relation to scale factor. I believe it holds also for any particle. I mentioned this some three years ago on the BAUT forums, where I worked on similar problems. (
linky) The reference given for explaining this decay of locally measured momentum is Misner, Thorne and Wheeler. I read MTW in small doses, because it goes well beyond my own level of expertise.
Cheers -- Sylas