oops, I am adding one more set of lines to the complete answer:
Author Andrew Beckwith wrote on May. 13, 2020 @ 01:03 GMTunstub
If the speed of light is a constant, i.e. normalizing it by having C = 1, then c^2= E/m is E=M and so then in that context the idea of a massive graviton would be congruent with emergent structure being pushed into a new universe. i.e. then we could say then that by Delta E times Delta t > or equal to hbar that again by Planck units we would have say
Delta E proportional to ( 1/ Delta t)
Set Delta E = Delta M, and then we have]
Delta M proportional to (1/delta t)
Does delta t = Planck time ?
I.e. avoiding a massless start would be consistent then with initial energy not equal to zero (in an emergent space-time structure), and if E = M with
Delta M = number of gravitons * (mass of a massive graviton)
However, does this mean that say we are restricted to Delta t, for a change in time being consistent with Planck time ?
Lets go to say that if c=1, (no varying speed of light), then the initial MASS of the universe may be, for Planck time delta t of the order of say
delta M directly proprtional to number of gravitons * (mass of a massive graviton)
It gets weirder than this.
In terms of indeterminacy of our analysis, how do we KNOW that c is the same speed of light, which we have today ?
If so then we do not know if our analysis of
Delta M is directly proportional to (Number of gravitons) * mass of massive Graviton
Nor do we know if
Delta M proportional to (1/ planck time) will allow us to scale
(number of gravitons) * (mass of a massive gravity graviton) ~ 1/ Planck time
We do not know this.
Experimental testing would be needed to determine or to ascertain if C=1 even in the initial phases of the universe
Secondly, as to the weight of the Universe, i.e. say E = M, if C=1 and we go forward say past planck time
Does M = [(Mass of gravitons )* Number of gravitons ] + say Dark Energy and or Dark mass ? ] if we assume there is an emergent structure of space time at the start of nucleation of the universe ?
Finally, does M if we are past planck time, go to 10^56 grams or so ?
i.e if and when do we get to the ? Present value of the mass of the Universe ?
All these questions are indeterminate and will live and die in terms of analysis if we have adequate data sets.
I hope this answers all the fantastic levels of indeterminacy which are out there, namely
A. Does C (speed of light remain constant always ? ).
B. Does the INITIAL Mass created by nucleation of the Universe
have proportionality to (number of gravitons)*(mass of a heavy graviton?)
C. When would the mass of the Universe , M ~ 10^56 grams ? or so
D. Is delta t, in the Above analysis restricted to planck time?
E. Can we say, if M~ 10^56 grams that we can still say use
M~ 10^56 grams ~ (number of gravitons)*(m for massive graviton) + [dark energy/dark matter ? ]
A, B, C, D, E would put a premium on rigorous testing and unless say we knew C= constant even at the start of the universe, then the problem as we initially have stated as to the initial WEIGHT of the Universe, or its energy equivalent may have no meaning in terms of answers.
Indeterminacy. How do we KNOW that C = a constant in ALL phases of evolution of the Universe ?
KEEP in mind that I am using delta E times delta t ~ 1 (h bar set = 1)
as a MINIMUM uncertainty
Indeciperability and indeterminacy
Recall if C= a constant that I proposed for delta t . If it is NOT always a constant, then we have NO way to do the analysis, via this thought exercise
Second level of indeterminacy,
Recall that for Delta t > Planck time that I wrote
delta M ~ (number of gravitons) * ( massive graviton mass) + [either dark matter/ and or Dark energy]
Recall the ELECTROWEAK transition in terms of cosmology, i.e. shortly after the big bang (if it occurred )
Do we have any idea of what forms
[either dark matter/ and or Dark energy] ?
Could the phase transition in the electroweak change the nature of the above ?
Also, keeping in mind , from Wikipedia
https://en.wikipedia.org/wiki/Electroweak_epoch
quot
e'
In physical cosmology, the electroweak epoch was the period in the evolution of the early universe when the temperature of the universe had fallen enough that the strong force separated from the electroweak interaction, but was high enough for electromagnetism and the weak interaction to remain merged into a single electroweak interaction above the critical temperature for electroweak symmetry breaking (159.5В±1.5 GeV [1] in the Standard Model of particle physics). Some cosmologists place the electroweak epoch at the start of the inflationary epoch, approximately 10в€'36 seconds after the Big Bang.[2][3][4] Others place it at approximately 10в€'32 seconds after the Big Bang when the potential energy of the inflaton field that had driven the inflation of the universe during the inflationary epoch was released, filling the universe with a dense, hot quark-gluon plasma.[5] Particle interactions in this phase were energetic enough to create large numbers of exotic particles, including stable W and Z bosons and Higgs bosons. As the universe expanded and cooled, interactions became less energetic and when the universe was about 10в€'12 seconds old, W and Z bosons ceased to be created at observable rates.[citation needed] The remaining W and Z bosons decayed quickly, and the weak interaction became a short-range force in the following quark epoch.
end of quote
That is a MASSIVE phase transtion
Finally, at what stage could we say
Delta M ~ M (mass of universe) ~ 10^56 grams ?
We do not have a clue YET
I hope this answers your question, Johnathan Dickau
Andrew Beckwith
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