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## Cosmological constant from first principles

Can the cosmological constant be derived from first principles? The answer appears to be - YES, according to this paper by Padmanabhan - 'The Physical Principle that determines the Value of the Cosmological Constant', http://arxiv.org/abs/1210.4174. This is, in part, an extension of Padmanabhan's earlier paper 'Emergent perspective of Gravity and Dark Energy', http://arxiv.org/abs/1207.0505.

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Recognitions:      Gold Member  There's a possible problem here: he's saying (I think) that λLF2 is ~1/nμ where n is the # of phase space cells within the Hubble radius (and μ turns out to be ~1.2). However, during the matter era, n $\propto$ ρ-3/4 $\propto$ t3/2, which would make λ variable. This is not allowed in GR. (When I say "# of phase space cells", I mean the # of photons that would result if all energy in the observable universe were converted to BB radiation.)

I'm not sure if I understood correctly, so please explain if I didn't...  But so it seems to me he says that there are three different phases of expansion: first de Sitter, then radiation dominated, then de Sitter again. If the Hubble parameter at first de Sitter phase is of order Planck mass, then the current Hubble parameter should be  $$H_{now} = \frac{a_{then}^2}{a_{now}^2} H_{then} = \frac{a_{then}^2}{a_{now}^2} L_P^{-1}$$ and since in de Sitter, cosmological constant is related to H, one gets $$\Lambda = 3H_{now}^2 = 3 \frac{a_{then}^4}{a_{now}^4} L_P^{-2}$$  Then he goes about calculating $Q = a_{now}/a_{then}$. I don't understand the calculation. There has to be some clear assumption for when the second de Sitter phase starts, and it has to be put in by hand. Where does the value fundamentally come from?

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## Cosmological constant from first principles

Quote by clamtrox 					 				 				I'm not sure if I understood correctly, so please explain if I didn't...  But so it seems to me he says that there are three different phases of expansion: first de Sitter, then radiation dominated, then de Sitter again. If the Hubble parameter at first de Sitter phase is of order Planck mass, then the current Hubble parameter should be  $$H_{now} = \frac{a_{then}^2}{a_{now}^2} H_{then} = \frac{a_{then}^2}{a_{now}^2} L_P^{-1}$$ and since in de Sitter, cosmological constant is related to H, one gets $$\Lambda = 3H_{now}^2 = 3 \frac{a_{then}^4}{a_{now}^4} L_P^{-2}$$  Then he goes about calculating $Q = a_{now}/a_{then}$. I don't understand the calculation. There has to be some clear assumption for when the second de Sitter phase starts, and it has to be put in by hand. Where does the value fundamentally come from?
The Hubble parameter during the inflationary epoch [1st de Sitter phase] is the Planck length [Lp]. The inflationary epoch is assumed to end when the de Sitter temperature is reached, defined as Tp = 1/(2piLp). This occurs at point D on p3 graph, the beginning of the radiation epoch. The radiation epoch ends when the number of comoving wave vectors that reenter the Hubble radius is the same as the number that exited during the inflationary epoch. This occurs at point B on p3 graph, which also marks the beginning of the second de Sitter phase. Q is the expansion factor, which is expected to be the same during all three epochs. It appears to me you can use the point when accelerated expansion began as the start of the second de Sitter phase.

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Quote by Chronos 					 				 				The Hubble parameter during the inflationary epoch [1st de Sitter phase] is the Planck length [Lp].
I suppose this depends on the chosen units and will be correct with everything expressed in Planck units, but then H_then = 1, not so?

Would Lp not be the Hubble radius, rather than the Hubble parameter, which would be extremely large, i.e. $H_{then} = 1/T_{Planck} \approx 10^{43} \, \, sec^{-1}$?

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Quote by Jorrie 					 				 				I suppose this depends on the chosen units and will be correct with everything expressed in Planck units, but then H_then = 1, not so?  Would Lp not be the Hubble radius, rather than the Hubble parameter, which would be extremely large, i.e. $H_{then} = 1/T_{Planck} \approx 10^{43} \, \, sec^{-1}$?
Agreed, the initial Hubble radius appears to be Lp, which expands by H~a during the inflationary epoch, followed by H~a^2 during the radiation epoch - which appears consistent with the LCDM model.

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Quote by Chronos 					 				 				Agreed, the initial Hubble radius appears to be Lp, which expands by H~a during the inflationary epoch, followed by H~a^2 during the radiation epoch - which appears consistent with the LCDM model.
I thought that during inflation (which is the 1st de Sitter phase), the Hubble radius remained constant and only started to grow when inflation ended (point D in Padmanabhan Fig.1). It is $\dot{a}$ that initially increased exponentially, but $H = \dot{a}/a$ remained constant. Or am I mixing things up the wrong way here?

Recognitions:      Gold Member        Science  Advisor  He calls the Hubble radius 'constant asymptotically' during inflation [p2], which lead me to assume H could increase linearly while 'a' went wild. It seemed logical, the modes within the initial Hubble radius would be whisked away, unable to reenter the Hubble radius until the radiation epoch commenced. The change in the Hubble radius during inflation may, however, be too trivial to be of any consequence.

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Quote by Chronos 					 				 				He calls the Hubble radius 'constant asymptotically' during inflation [p2], which lead me to assume H could increase linearly while 'a' went wild.
Thanks, makes sense. Sharp slope changes on log-log plots are really gradual changes on linear plots.

From his page 7, second bullet:

Time translation invariance of the geometry suggests that de Sitter space-  time qualiﬁes as some kind of “equilibrium” conﬁguration.  Given the two  length scales, one can envisage two de Sitter phases for the universe, one  governed by H  = Lp−1  and the other governed by H  = (Λ/3)1/2.  Of these,   I would expect the Planck scale inﬂationary phase to be an unstable equi-  librium causing the  universe to make a transition towards the  second de  Sitter  phase  governed by the  cosmological constant. The  transient stage  is populated by matter emerging along with classical geometry around the  point D in Fig. 1.

I don't quite catch the meaning of the last sentence. Does he mean that all the radiation and matter (energy) that we observe emerged around point D, or did it gradually emerge during the middle phase (D to B), i.e. migrated from the left side of the parallelogram to the right side? We are presumable situated very near point B, busy entering phase B to C.
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Recognitions:      Gold Member        Science  Advisor  Me neither. The emergent phase is not well characterized. It appears he asserts a quantum gravity solution is required on that count.

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