Cosmic Entropy Prediction with Extremely High Precision in Rh = ct Cosmology

1. Black Hole $R_h=ct$ Cosmology Model Entropy

Herein we will mainly focus on $R_h=ct$ cosmology, which covers a group of cosmology models actively discussed as an alternative to the $\Lambda$-CDM model; see, for example, [2,3,4,5,6,7]. Melia [8,9] has recently compared many different kinds of observation with respect to the $\Lambda$-CDM and $R_h=ct$ models, and concludes that “$R_h=ct$ has accounted for the data at least as well as the standard model, and often much better.” Nevertheless, it remains to be determined by the cosmology community which model will ultimately prevail.

There are multiple types of cosmological models following the $R_h=ct$ principle, namely, linear growth of the universal radius at the speed of light. In this paper, the type of $R_h=ct$ model of interest is growing black hole $R_h=ct$ cosmology, within which black hole entropy can be explored.

As early as 1972, Pathria [10] pointed out that the Hubble sphere has mathematical properties similar to those of a black hole. See, for example, [6,11,12,13,14,15]. Herein our focus will be on a Schwarzschild black hole universe model following a linear $R_h=ct$ expansion. Accordingly, our model entropy follows the Bekenstein-Hawking black hole entropy formula [16,17,18].

The Bekenstein-Hawking entropy is given by:

$$S_{BH}={\displaystyle \frac{A}{l_p^2}}={\displaystyle \frac{4\pi R_s^2}{l_p^2}}$$

(1)

In a critical Friedmann [19] universe, the mass is equal to $M_c={\displaystyle \frac{c^2{R}_H}{2G}}$. If we solve this for $R_H$, we get $R_H={\displaystyle \frac{2G{M}_c}{c^2}}$. In other words, the Hubble radius and the Schwarzschild radius are identical in a critical Friedmann universe. If our universe is also following a linear $R_h=ct$ expansion, and is a growing Schwarzschild black hole, then its entropy can presumably be treated as:

$$S_{BH}={\displaystyle \frac{A}{l_p^2}}={\displaystyle \frac{4\pi R_H^2}{l_p^2}}$$

(2)

As early as 2015, Tatum et al. [20] suggested the following formula for the Cosmic Microwave Background (CMB) radiation temperature consistent with a growing black hole $R_h=ct$ model and the critical Friedmann universe:

$$T_{cmb}={\displaystyle \frac{\hslash c}{k_{b}4\pi \sqrt{R_{h}2l_p}}}$$

(3)

wherein $k_b$ is the Boltzmann constant, ℏ is the reduced Planck constant (the Dirac constant), and $R_h={\displaystyle \frac{c}{H_0}}$. Haug and Wojnow [21,22] have demonstrated that this formula can be derived from the Stefan-Boltzmann law. Furthermore, Haug and Tatum [23] have shown that the same formula can be derived using a geometric mean approach, and Haug [24] has also demonstrated that it can be derived from the quantization of light bending.

If one solves formula (3) for $H_0$, this gives:

$$H_0=T_{cmb}^2{\displaystyle \frac{k_b^{2}32{\pi }^2{l}_p}{{\hslash }^{2}c}}$$

(4)

This means that we can rewrite the Bekenstein-Hawking entropy as:

$$S_{BH}={\displaystyle \frac{A}{l_p^2}}={\displaystyle \frac{4\pi R_H^2}{l_p^2}}={\displaystyle \frac{1}{T_{cmb}^4}}{\displaystyle \frac{{\hslash }^4{c}^4}{256{\pi }^3{k}_b^4{l}_p^4}}$$

(5)

And, since we know that the Planck [25] time is given by $t_p=\sqrt{{\displaystyle \frac{G\hslash }{c^5}}}={\displaystyle \frac{l_p}{c}}$, this entropy can also be written as:

$$S_{BH}={\displaystyle \frac{A}{l_p^2}}={\displaystyle \frac{4\pi R_H^2}{l_p^2}}={\displaystyle \frac{1}{T_{cmb}^4}}{\displaystyle \frac{{\hslash }^4}{256{\pi }^3{k}_b^4{t}_p^4}}$$

(6)

Be aware that the Planck time can be found independent of first finding G; see [26,27]. However, we can also re-write this in a form containing G; in which case, we then have:

$$S_{BH}={\displaystyle \frac{A}{l_p^2}}={\displaystyle \frac{4\pi R_H^2}{l_p^2}}={\displaystyle \frac{1}{T_{cmb}^4}}{\displaystyle \frac{{\hslash }^2{c}^{10}}{256{\pi }^3{k}_b^4{G}^2}}$$

(7)

The above formula expressing the Bekenstein-Hawking entropy as a function of the CMB temperature was first presented by Tatum and Seshavatharam in 2018 [1]. In the current paper, we will demonstrate how such a temperature formula leads to an incredibly low STD for the predicted Hubble sphere entropy.

This new way to express the Schwarzschild black hole entropy is more than just a change of the elements in which it is expressed; there are also important practical implications for cosmology, since the CMB temperature has been measured much more precisely than the Hubble constant. For example, Dhal et al. [28] report a CMB temperature of $2.725007\pm 0.000024K$. This leads to a Hubble sphere $R_h=ct$ black hole entropy of $S_{BH}=9.2057\pm 0.0007\times {10}^{122}$. We even account for the uncertainty in the Planck length, which is needed to calculate the Bekenstein-Hawking entropy, using the NIST CODATA value of $l_p=1.616255\pm 0.000018\times {10}^{-35}m$.

Table 1 shows Bekenstein-Hawking entropies estimated using the CMB temperature measured in recent studies [28,30,31]. Table 2 shows Bekenstein-Hawking entropies estimated using $H_0$ values from recent studies [32,33,34,35]. We clearly see that our new CMB entropy method is much more precise in comparison to the Hubble constant entropy method. In addition, there is what may be referred to as an entropy tension between different $H_0$ studies, somewhat similar to the well-known Hubble tension. However, this is outside the scope of of our present paper. See also [29].

Haug [36] has recently demonstrated that the number of quantum operations since the Planck epoch in a critical Friedmann universe following linear $R_h=ct$ black hole cosmolology is given by:

$$\#ops\approx {\displaystyle \frac{S_{BH}}{8\pi }}$$

(8)

This means that, using the Dhal CMB temperature study, for example, formula (8) would imply that the number of such operations is $3.6628\pm 0.0003\times {10}^{122}$. The magnitude of this number is quite interesting, because of its remarkable similarity to that of the well-known cosmological constant problem.

2. The Schwarzschild Metric for a Hubble Sphere Black Hole Written in Entropy Form

The Schwarzschild [37] metric is normally given by:

$$d{s}^2=-\left(1-{\displaystyle \frac{2GM}{r{c}^2}}\right)c^{2}d{t}^2+{\left(1-{\displaystyle \frac{2GM}{r{c}^2}}\right)}^{-1}d{r}^2+r^2{\Omega }^2$$

(9)

Since we have:

$$S_{BH}={\displaystyle \frac{A}{l_p^2}}={\displaystyle \frac{4\pi r_s^2}{l_p^2}}={\displaystyle \frac{4\pi 4G^2{M}^2}{c^4{l}_p^2}}$$

(10)

we can now solve this for $GM$ and get: $GM={\displaystyle \frac{c^2{l}_p}{4}}\sqrt{{\displaystyle \frac{S_{BH}}{\pi }}}$. This means that, for a black hole, the Schwarzschild metric can be re-written as a function of the black hole Bekenstein-Hawking entropy. We then get:

$$\begin{array}{ccc}\hfill d{s}^2& =& -\left(1-{\displaystyle \frac{2GM}{r{c}^2}}\right)c^{2}d{t}^2+{\left(1-{\displaystyle \frac{2GM}{r{c}^2}}\right)}^{-1}d{x}^2+r^2{\Omega }^2\hfill \\ \hfill d{s}^2& =& -\left(1-{\displaystyle \frac{l_p}{2r}}\sqrt{{\displaystyle \frac{S_{BH}}{\pi }}}\right)c^{2}d{t}^2+{\left(1-{\displaystyle \frac{l_p}{2r}}\sqrt{{\displaystyle \frac{S_{BH}}{\pi }}}\right)}^{-1}d{x}^2+r^2{\Omega }^2\hfill \end{array}$$

(11)

This is of great interest, since it shows that the black hole metric can now be expressed in terms of the Planck length and Bekenstein-Hawking entropy. Eddington [38] was the first to suggest that the Planck scale would likely play an important role in a future quantum gravity theory, see also [22].

3. The Critical Friedmann Equation

The critical Friedmann equation is given by:

$$H_0^2={\displaystyle \frac{8\pi G\rho }{3}}$$

(12)

This can now be re-written to include the Bekenstein-Hawking entropy, the Planck length and the speed of light according to:

$$\begin{array}{ccc}\hfill H_0^2& =& {\displaystyle \frac{8\pi G\rho }{3}}\hfill \\ \hfill H_0^2& =& {\displaystyle \frac{c^6}{4G^2{M}^2}}\hfill \\ \hfill H_0^2& =& {\displaystyle \frac{4c^2\pi }{l_p^2{S}_{BH}}}\hfill \\ \hfill H_0& =& {\displaystyle \frac{2c}{l_p}}\sqrt{{\displaystyle \frac{\pi }{S_{BH}}}}\hfill \end{array}$$

(13)

See also [39,40] for more background, including parallels to this, such as our new thermodynamic Friedmann equation.

There is much yet to be learned about how the thermodynamic concept of entropy might apply to the observable universe and to black holes in general. This subject becomes especially relevant with respect to growing black hole models of cosmology. What effect cosmic entropy might have on the phenomena associated with gravity needs to be further explored. The holographic principle, when applied to the universe as a finite global object, is a related subject of great interest, although beyond the scope of the present brief communication.

4. Conclusions

Due to recent theoretical progress in understanding the direct mathematical relationship between the CMB temperature and the Hubble constant, we can now also estimate the Hubble sphere entropy directly from the CMB temperature. Since the CMB temperature is measured much more precisely than the Hubble constant, this allows for a much more accurate and precise estimate of the entropy of the Hubble sphere black hole $R_h=ct$ universe than previously presented. There are remarkable similarities between the magnitude of the cosmic entropy calculated in the present paper and the magnitude of the cosmological constant problem [40]. This poses interesting questions for continuing theoretical investigations, including those which apply the cosmological holographic principle.