Quantum postNewtonian theory for corpuscular Black Holes
Abstract
We discuss an effective theory for the quantum static gravitational potential in spherical symmetry up to the first postNewtonian correction. We build a suitable Lagrangian from the weak field limit of the EinsteinHilbert action coupled to pressureless matter. Classical solutions of the field equation lead to the correct postNewtonian expansion. Furthermore, we portray the Newtonian results in a quantum framework by means of a coherent quantum state, which is properly corrected to accomodate postNewtonian corrections. These considerations provide a link between the corpuscular model of Dvali and Gomez and standard postNewtonian gravity, laying the foundations for future research.

Arnold Sommerfeld Center, LudwigMaximiliansUniversität, Theresienstraße 37, 80333 München, Germany

Email: A.Giugno@physik.unimuenchen.de
1 Introduction
Newtonian theory describes gravity in terms of forces, allowing to welldefine energy and to provide the existence of a related scalar potential. On the other hand, to specify these quantities in General Relativity (GR) proves to be a harder task, since it characterizes the gravitational field through the local geometry of spacetime [1]. Therefore, the notion of a scalar potential is not univocal for any observer. In the postNewtonian approximation, the local curvature is weak and the velocities of any test particle are nonrelativistic, which supports the derivation of an effective theory for the gravitational potential generated by static and isotropic compact sources. This formulation sees the approximated geodesic equation as a standard Newton’s law, whose potential is in turn determined by the Poisson equation. We further enrich the picture by adding nonlinearities in the quantum interpretation of the gravitational potential [2], in the light of the results of Ref. [3]. It is important to stress out that this “Newtonianlike" approach is one of the fundamental ingredients, which allow to quantise gravitational degrees of freedom with standard methods [4, 5, 6, 7, 8], once some properties like spherical symmetry are implied. The conceptual arena where this study is carried on, is the corpuscular model of gravity brought to light by Dvali and Gomez [9, 10, 11, 12, 13]. A black hole is naturally formed by a large number of gravitons, which superimpose in the same quantum state and hence realise a BoseEinstein Condensate (BEC) stably on the verge of a quantum phase transition [14, 15, 16, 17, 18, 19, 20]. In addition to that, the gravitons are expected to be marginally bound in their (gravitational) confining potential well [21, 22, 23], whose size is set by the distinctive Comptonde Broglie wavelength , where
(1) 
is the gravitational radius of the black hole of ADM mass , and whose depth is directly proportional to the number of soft quanta [24, 25, 26, 27, 28]. We mention here that we shall work in units of the Planck length and mass , so that the Newton constant reads , while . The speed of light is instead normalised to .
Although the original outline [12] only took the degrees of freedom of gravity into consideration, especially when is of astrophysical size [29, 30, 31], and substantially neglected the contributions of collapsing baryonic matter, the postNewtonian approximation [3] emerges in a simple fashion when they are properly taken into account. The concept is straightforward: let us pretend to have baryons of rest mass very far apart, with their total ADM mass [32] thus given by . During the gravitational collapse, the baryons are enclosed in a sphere of radius and possess a (negative) gravitational energy , where is the associated Newtonian potential. On a quantum mechanical perspective, the link with the classical potential is achieved thanks to the expectation value of a scalar field , , over a coherent state . This feature entails that the graviton number is determined by the normalisation of the coherent state and follows Bekenstein’s area law [33], , when . Moreover, the Comptonde Broglie length is recovered through the assumption that it is the wavelength of almost the entire amount of gravitons. Thus, the (negative) energy of any constituent yields consistently and the graviton selfinteraction energy, reproduces the typical postNewtonian correction. It is easy to match this machinery with the standard knowledge. Considering indeed a star of size we get , whereas we recover the socalled “maximal packing” condition of Ref. [9],
(2) 
when gravity is strongly coupled, i.e. .
In the following, we first derive a consistent effective theory for a static and spherically symmetric potential by considering the EinsteinHilbert action in the aforementioned nonrelativistic and weak field regimes. The inclusion of NexttoLinear Order (NLO) terms provides classical results in compliance with the usual postNewtonian expansion of the Schwarzschild metric. Furthermore, the quantum state of the soft scalar gravitons is correctly represented by a coherent state, which establishes a link between a microscopic description of gravity and the macroscopic geometry of spacetime. Therefore, such an outcome [2] enriches and improves the conclusions of Ref. [3].
2 Classical effective theory
In order to build a correct effective theory, we first have to show how a real scalar field can describe the postNewtonian approximation of the weak field limit of Schwarzschild metric [1]. The reader shall bear in mind, however, that this construction assumes that a specific reference frame has been chosen. The starting point of our discussion is the EinsteinHilbert action
(3) 
coupled to the Lagrangian density that represents the ordinary matter, which collapses and acts as a source for the graviational field. We labeled the Ricci scalar with . As we already stressed out, in order to retrieve the wellknown postNewtonian result the local curvature has to be small, which means that the metric can be expanded as , where , and . Moreover, the characteristic velocity of the matter under consideration is many orders of magnitude smaller than the speed of light in the considered reference frame . We can safely describe the entire gravitational system through one relevant component of , , which is also timeindependent. The stressenergy tensor is hence completely specified by the nonrelativistic energy density, , where represents the fourvelocity of the constituents of the source. Furthermore, this tensor allows to choose the matter Lagrangian simply as , which is enough to our purpose, since we suppose that matter pressure is negligible [34, 35] and we neglect the associated dynamics. We can finally make the identification , since the the Newtonian potential is known to satisfy the Poisson equation
(4) 
while the de Donder gauge fixing takes the very simple form . It is now straightforward to introduce an effective scalar field theory for the gravitational potential. To do so, we first insert in the EinstenHilbert action, and then we compute the related Hamiltonian by making a Legendre transformation of the Lagrangian . Then, we include nonlinearities through the introduction of a selfgravitational source, defined as a the gravitational potential energy per unit volume. Leaving a more detailed analysis of such a construction to Ref. [2] (and the Appendices thereof, in particular), here we only report the resulting Lagrangian
(5) 
The couplings and measure the strength of the interaction of with baryonic matter and the selfsourcing, respectively. They are rescaled in such a way to recover the known postNewtonian expansion for . The EulerLagrange equation for is given by
(6) 
and it is obviously hard to solve analytically for a general source. We will therefore expand the field up to first order in the coupling , , and solve Eq. (2) order by order. In particular, for the leading order we have the analog of the Poisson Eq. (2), while
(7) 
gives the correction at . To linear order in , the onshell Hamiltonian reads
(8) 
If we take e.g. a matter distribution uniformly distributed within a sphere of radius [2], not only the solution of the field Equation correctly reproduces the potential that one expects in semiclassical gravity, but also the potential energy computed thanks to Eq. (2) reads
(9) 
being again the ADM mass sourcing the graviational field up to order . It is of paramount importance to notice that vanishes when , realising therefore the “maximal packing" condition (1).
3 Quantum realisation
In order to canonically quantise the theory, we consider the rescaled real scalar field , coupled to the static source and replace these new quantities in Eq. (2). We straightforwardly obtain the scalar field Lagrangian
(10) 
where we again assumed . Let us look for a wavefunction which reproduces the classical solution of the EOM of . First, we examine the linear case, . In terms of the new variables and , it is analogous to a Poisson Equation when the field is static as its own source. Upon expanding the EOM on a base of spherically symmetric normal modes, one can solve this Equation in momenta space, so that
(11) 
A shift transformation of the ladder operators related to shows that the coherent state correctly reproduces the classical solution, , with
(12) 
and . It is possible to read off the mean number of quanta from the normalisation condition , which turns out to be
(13) 
and is shown to precisely equal the total occupation number of modes in the state . For a uniform source of finite size and ADM mass , this amount can be estimated as
(14) 
where is a IR cutoff, which cures the divergence coming from embedding a static (and eternal) field in an infinite spacetime. In reference to that, it is interesting to point out that the dependence of is weaker on than on the mass , since
(15) 
and allows to recover the opening result when is arbitrarily large. We can now add the nonlinearity described by Eq. (2), rewritten as
(16) 
so that
(17) 
is a diverging contribution coming from the vacuum, which can be removed through normal ordering in the expectation value. By means of Eq. (3), one can immediately see that equals the classical expression, that is
(18) 
for any current sourcing the scalar field. The coherent state is therefore an appropriate basis for a perturbative analysis in Quantum Field Theory. In order to refine the result, one shall find a modified coherent state , such that
(19) 
to first order in . As for the classical potential in Eq. (2), we can expand the quantum state as , where is a normalisation constant. After manipulating Eq. (3) with some cumbersome algebra [2], we succeed in relating the correction to any eigenvalue, , to the entire set of ’s, i.e.
(20) 
Of course, this Equation is very complicated and any attempt to deal with it without some sort of approximation is destined to fail. Therefore, we follow the argument outlined in Refs. [3, 15] and pretend that almost the whole set of toy gravitons belongs to one mode of wavelength [9], so that one can finally identify [2]
(21) 
where . Considering e.g. the pointlike source of Ref. [2], one obtains
(22) 
with the help of a UV cutoff , that removes the infinities coming from the vanishing spatial extension of the source. When the result falls within the range of validity of our approximation, that is , we see that the perturbation correctly enjoys the relation , which is compatible with the classical result that we want to extend to the domain of quantum physics.
4 Conclusions and outlook
We have constructed an effective quantum theory for the gravitational potential sourced by a static matter distribution and up to first postNewtonian order, by approximating the EinsteinHilbert action in the weak field and nonrelativistic regimes. The result [2] implies the maximal packing condition (1), which is a signature feature of the corpuscular BH model of Dvali and Gomez [12]. Furthermore, we refined the expression (3) for the total number of soft quanta, , forming the selfsustained BEC and we showed that it is not only influenced by the total ADM mass of the black hole as in standard literature [13], but also encodes more information, albeit to a much weaker extent. In fact, the logarithmic dependence on the ratio becomes more and more negligible as the system approaches an ideal configuration, for which , while it is expected to give a nontrivial contribution in a dynamical situation. Moreover, we stated several times that our analysis looses accuracy for a source of size , as we have shown that the consistency relation gets spoiled as one moves further away from it. Still, it would be interesting to investigate the case where the inequality is saturated, that is , since Eq. (1) arises precisely in this regime and allows the black hole to be selfsustained. The possible outcome may be able to quantify the departure of the present analysis from the standard postNewtonian approximation of GR, possibly providing some glimpses of a full theory of Quantum Gravity. In addition to that, it is necessary to understand the role of matter pressure, which has been completely neglected so far, but may have important cosmological implications [37, 38].
Acknowledgments
This proceeding is based on a series of papers in collaboration with R. Casadio, A. Giusti and M. Lenzi. The author is partially supported by the ERC Advanced Grant 339169 "Selfcompletion". This work has also been carried out in the framework of activities of the National Group of Mathematical Physics (GNFM, INdAM).
References
References
 [1] Weinberg S 1972 Gravitation and Cosmology: Principles and Applications of the General Theory of Relativity (New York: Wiley and Sons)
 [2] Casadio R, Giugno A, Giusti A and Lenzi M 2017 Phys. Rev. D 96 no.4, 044010
 [3] Casadio R, Giugno A and Giusti A 2016 Phys. Lett. B 763 337
 [4] Duff M J 1973 Phys. Rev. D 7 2317
 [5] Donoghue J F, Ivanov M M and Shkerin A 2017 Preprint arXiv:1702.00319 [hepth]
 [6] Casadio R, Giugno A and Giusti A 2017 Gen. Rel. Grav. 49 no.2, 32
 [7] Casadio R, Giugno A and Micu O 2016 Int. J. Mod. Phys. D 25 no.02, 1630006
 [8] Giusti A 2017 Preprint arXiv:1709.10348 [grqc]
 [9] Dvali G and Gomez C 2014 JCAP 01 023
 [10] Dvali G and Gomez C 2014 Eur. Phys. J. C 74 2752
 [11] Dvali G and Gomez C 2013 Phys. Lett. B 719 419
 [12] Dvali G and Gomez C 2012 Phys. Lett. B 716 240
 [13] Dvali G, Gomez C and Mukhanov S 2011 Preprint arXiv:1106.5894 [hepph]
 [14] Flassig D, Pritzel A and Wintergerst N 2013 Phys. Rev. D 87 084007
 [15] Casadio R, Giugno A, Micu O and Orlandi A 2014 Phys. Rev. D 90 084040
 [16] Casadio R, Giugno A and Orlandi A 2015 Phys. Rev. D 91 124069
 [17] Casadio R, Giugno A, Micu O and Orlandi A 2015 Entropy 17 6893
 [18] Kühnel F 2014 Phys. Rev. D 90 084024
 [19] Kühnel F and Sundborg B 2014 JHEP 1412 016
 [20] Kühnel F and Sundborg B 2014 Phys. Rev. D 90 064025
 [21] Casadio R and Orlandi A 2013 JHEP 1308 025
 [22] Mück W and Pozzo G 2014 JHEP 1405 128
 [23] Casadio R, Giugno A, Giusti A and Micu O 2017 Eur. Phys. J. C 77 no.5, 322
 [24] Ruffini R and Bonazzola S 1969 Phys. Rev. 187 1767
 [25] Colpi M, Shapiro S L and Wasserman I 1986 Phys. Rev. Lett. 57 2485
 [26] Membrado M, Abad J, Pacheco A F and Sanudo J 1989 Phys. Rev. D 40 2736
 [27] Nieuwenhuizen T M 2008 Europhys. Lett. 83 10008
 [28] Chavanis PH and Harko T 2012 Phys. Rev. D 86 064011
 [29] Dvali G and Gußmann A 2016 Nucl. Phys. B 913 1001
 [30] Dvali G and Gußmann A 2017 Phys. Lett. B 768 (274279
 [31] Kühnel F and Sandstad M 2015 Phys. Rev. D 92 124028
 [32] Arnowitt R L, Deser S and Misner C W 1959 Phys. Rev. 116 1322
 [33] Bekenstein J D 1973 Phys. Rev. D 7 2333
 [34] Madsen M S 1988 Class. Quant. Grav. 5 627
 [35] Brown J D 1993 Class. Quant. Grav. 10 1579
 [36] Harko T 2010 Phys. Rev. D 81 044021
 [37] Casadio R, Giugno A and Giusti A 2017 Preprint arXiv:1708.09736 [grqc]
 [38] Cadoni M, Casadio R, Giusti A, Mück W and Tuveri M 2017 Preprint arXiv:1707.09945 [grqc]