I've asked this question once; want to be more specific now; hope will be luckier this time around. According to the original Gamov-Alpher-Hermann theory, the CMB temperature goes down with time "t" as t^(-2/3). A recent discovery of accelerated expansion of the Universe apparently is changing this. So what is a new dynamics of that temperature?
Remi, thanks for your "do-it-yourself" advice, but I'd rather prefer a direct answer or better-- a good reference.
Anna, great thanks; I'll be reading that article carefully, although my first impression is that the number I am looking for isn't there. I can make my own calcs, of course, but it is not my main subject of interest, and I'd rather rely on a good direct reference for my research and paper without citing my own "home cookie" number if the answers are in the literature. But the paper supplied by you is really interesting, and anyway, I can now get in touch with its author and burden him with my request for reference:-).
According to thermodinamics T is inversely proportional to the scale factor, In the standard model previous to SNe1A "accelerating" universe your equation was considered right. Now, a more complex behaviour as emerged as standard. From my own work, the steady flow model, you get T inversely proportional to t for almost the entire history of the Universe, with some interesting implications...
Juan, thanks. Sound great; can you provide a reference or even better -- a link to that paper of yours?
Juan:
Yes, thanks, I have seen it already. By now, after reading Weinberg book (2008) and Caldwell review (2009), where as I can see most of theories presume that radiation and dark energy densities are time-invariant, I am sort of content to see how their time dependence can be put into play. I'll read it in more detail later on. I know by now that the time dependence I am looking for, varies pretty much on which type of density is dominant in the universe (say from T ~ t^(-2/3) for "old" model (non-relativistic mass-energy), to T ~ t^(-1/2) for radiation energy dominance, and your model produces a whooping T ~ t^{-1}. Was there any discussion in the literature of that model of yours?
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