SemiHolography for Heavy Ion Collisions: SelfConsistency and First Numerical Tests
Abstract
We present an extended version of a recently proposed semiholographic model for heavyion collisions, which includes selfconsistent couplings between the YangMills fields of the Color Glass Condensate framework and an infrared AdS/CFT sector, such as to guarantee the existence of a conserved energymomentum tensor for the combined system that is local in space and time, which we also construct explicitly. Moreover, we include a coupling of the topological charge density in the glasma to the same of the holographic infrared CFT. The semiholographic approach makes it possible to combine CGC initial conditions and weakcoupling glasma field equations with a simultaneous evolution of a strongly coupled infrared sector describing the soft gluons radiated by hard partons. As a first numerical test of the semiholographic model we study the dynamics of fluctuating homogeneous colorspinlocked YangMills fields when coupled to a homogeneous and isotropic energymomentum tensor of the holographic IRCFT, and we find rapid convergence of the iterative numerical procedure suggested earlier.
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1 Introduction
Describing the full time evolution and equilibration process of the fireball created in ultrarelativistic heavyion collisions is an extremely difficult task due to the interplay of perturbative and nonperturbative phenomena. Tracing the full evolution appears to require a patchwork of different effective theories, each designed to describe a certain stage of the evolution and only applicable to specific physical observables.
According to the color glass condensate (CGC) framework Gelis:2010nm (), at very early times the system is dominated by gluons with typical momenta of the order of the semihard saturation scale , which are relatively weakly coupled (when is large), , but which have high occupation numbers . This admits a description in terms of semiclassical YangMills fields, also called the glasma Lappi:2006fp (), which has been studied by numerical solutions of classical YangMills equations Romatschke:2006nk (); Gelis:2013rba (); Berges:2013fga (). As the system undergoes rapid longitudinal expansion and the occupation number of the semihard gluons drops, soft gluons are emitted abundantly, whose dynamics is characterised by a significantly larger coupling . This growing soft sector is presumed to play a crucial role in the evolution of the whole system.
While the rapid thermalization suggested by experimental data might be captured by an effective kinetic theory description extrapolated to strong coupling Kurkela:2015qoa (), insight into isotropization and thermalization of a strongly coupled quantum field theory can be comparatively directly gained by gauge/gravity duality. The latter maps the thermalization process to black hole formation in asymptotically antide Sitter space DeWolfe:2013cua (); Chesler:2013lia (). By comparing results from hydrodynamic simulations with the full holographic evolution it was found that the system is accurately described by hydrodynamics although large viscous corrections are still present. Later the system isotropizes and reaches local thermal equilibrium Chesler:2010bi (); Heller:2011ju (). (For an extensive list of references see the recent review Chesler:2015lsa ().)
The mechanism how the initial state makes a transition to a state that is amenable to a hydrodynamic description is however different for weak and strong coupling (although quantitatively there might exist a smooth interpolation Keegan:2015avk ()). At asymptotically high energies and parametrically small coupling the thermalization pattern is of the bottomup type Baier:2000sb (); Kurkela:2011ub (), where first the soft gluons form a thermal bath which then draws energy from the hard modes. On the other hand, at infinite coupling the thermalization process as obtained via the gauge/gravity correspondence is topdown, meaning that highly energetic modes reach their thermal distribution first Balasubramanian:2011ur (). By considering corrections to the infinitecoupling limit it was shown in Steineder:2012si (); Stricker:2013lma () that there indeed exists a transition between the two behaviors at intermediate coupling.
A description of the whole evolution from within a single framework and from first principles is elusive at this point. So far most studies have either utilized solely a weakly coupled approach or a strongly coupled one, but in order to understand the evolution of the colliding matter better, one needs to combine the different effective descriptions for the different stages as well as weak and strong coupling phenomena. In recent years various attempts in this direction have been made. For example, in vanderSchee:2013pia () different effective descriptions were patched together. The farfromequilibrium initial stage was simulated by colliding shock waves using numerical AdS/CFT, whose results were used as an input for the hydrodynamic evolution, which subsequently served as an input for the kinetic theory describing the low density hadronic stage.
However, the initial conditions set up for AdS/CFT calculations, even in stateoftheart shockwave collisions, have no clear connection to those derived directly from (weakcoupling) QCD in the (nonperturbative) CGC framework. It would seem highly desirable to be able to connect the two approaches and follow the combined evolution of weakly coupled semihard gluons and a strongly interacting soft sector.
The first semiholographic proposals for describing interactions between a weakly coupled and a strongly coupled sector, where the strongly coupled sector is described by a holographic dual, were made in the context of nonFermi liquids Faulkner:2010tq (); Mukhopadhyay:2013dqa (). In the context of heavyion collisions one attempt to combine weak and strong coupling was made in a socalled hybrid approach to describe the energy loss of jets moving through a strongly coupled medium CasalderreySolana:2014bpa (), where the soft inmedium effects were modeled by using insights from gauge/gravity duality. However, in this case no back reaction of the soft medium to the hard partons was taken into account.
A different route was recently taken in Iancu:2014ava () where a semiholographic model for thermalization in heavyion collisions was presented. This model is able to incorporate the interaction between weakly coupled hard and strongly coupled soft modes but so far lacks verification by carrying out a concrete calculation. The goal of this work is to refine and test the proposal of Iancu:2014ava () with regard to its internal selfconsistency and numerical practicability (while not yet attempting to shed new light on thermalization in heavyion collisions).
The outline of this paper is as follows. In Sec. 2 we review and also extend the semiholographic model of Iancu:2014ava (). Specifically, we present a reformulation of the model which permits the definition of a locally conserved energymomentum tensor of the combined system of hard and soft degrees of freedom. In Sec. 3 we present a simple test case for semiholographic glasma evolution. We truncate the couplings of the model developed in Sec. 2, such that only gravitational degrees of freedom are excited in the holographic sector and moreover impose homogeneity and isotropy in both the hard and the soft sector. As a consequence the (timedependent) gravity dual of this test case can be treated analytically, but due to the Birkhoff theorem does not allow for dynamical blackhole formation or perturbation. Thus, the soft degrees of freedom captured by the dual strongly coupled field theory cannot equilibrate with the hard degrees of freedom, i.e., this simple test case is too restricted for permitting to study thermalization. It however allows us to carry out a first proofofprinciple calculation, where we can verify the convergence of an iterative numerical solution of the semiholographic setup. Section 4 contains our conclusions and an outlook.
2 Action and energymomentum tensor of the semiholographic setup
Following Iancu:2014ava (), in this section we construct an action where the description of a semihard gluon (UV) sector and that of a stronglyinteracting soft gluon (IR) sector can be coupled selfconsistently. In this paper, we will treat the semiholographic model phenomenologically including minimalistic hardsoft couplings only, without attempting a derivation from first principles; a rigorous framework for a possible derivation has been recently proposed in Behr:2015aat ().
The assumptions that provide the basis of the semiholographic model for heavyion collisions in Iancu:2014ava () are as follows:

the overoccupied semihard (UV) gluons allow for a description in terms of a classical Yang–Mills theory as in the glasma model Gelis:2010nm (); Lappi:2006fp (),

the infrared sector is described by a conformal field theory (IRCFT) which is approximated by the strongcoupling large limit such that a classical dual holographic description is possible,

the IRCFT is marginally deformed such that its marginal couplings become functionals of the color fields of the glasma, while the marginal operators of the infrared conformal field theory (IRCFT) appear as selfconsistent fields which modify the classical YangMills dynamics of the color fields of the glasma, and

the hardsoft couplings describing the mutual feedback between the IRCFT and the color fields of the glasma involve local gaugeinvariant operators of both sectors, and the coupling constants are given by a dimensionless number times , with being the saturation scale of the colliding nuclei.
In addition to the proposal in Iancu:2014ava () we demand a well defined action principle that allows for the construction of a conserved energymomentum tensor for the combined system living in flat space.
For the action describing the interactions between the hard and soft modes, which satisfies all the criteria mentioned above, we propose
(1) 
which we will discuss now in detail.
We start with the YangMills part of the action and for the time being, consider a classical YangMills theory living on an arbitrary nondynamical background metric , which in the end will be set to the flat Minkowski metric. This is for technical purposes only because it is convenient for identifying the tensorial properties of the variables to be defined below. The YangMills action in this background is given by
(2) 
We use the normalisation for the generators of the gauge group together with the standard convention for the covariant derivative , where is the LeviCivita connection with respect to .
The gauge invariant operators of the UV sector used to deform the IRCFT are , the energymomentum tensor of the YangMills fields, , which takes the standard form
(3) 
and the YangMills Pontryagin density
(4) 
Notice that , as well as are functionals of the background metric .
The second part of the action (1), , is the generating functional of the IRCFT, provided by the onshell gravitational action of its gravity dual. The gravitational dynamics will be described by Einstein’s gravity with asymptotically AdS boundary conditions minimally coupled to matter.^{1}^{1}1It is to be noted that the AdS radius does not explicitly appear in the IRCFT variables in the strong coupling and large limit. The parameter which gives higher derivative corrections to Einstein’s gravity is identified with (up to a numerical factor) where is the analogue of the ’t Hooft coupling of the IRCFT. This disappears when we take the limit . The factor is proportional to , where is the analogue of the rank of the gauge group of the IRCFT. This should be parametrically of the same magnitude as the of QCD—the relative numerical factor can be absorbed in the definitions of the hardsoft coupling constants given below. However, at this point we can be completely agnostic about the IRCFT generating functional , meaning that we do not need to know its explicit form in terms of the elementary fields. We only need that describes a marginally deformed CFT in presence of three background sources, namely , and , which couple to the three marginal operators of dimension , namely (the energymomentum tensor of the CFT), (the glueball/Lagrangian density operator of the CFT) and (the topological charge density operator of the CFT), respectively^{2}^{2}2To be consistent with the notation in Iancu:2014ava (), we denote IRCFT operators by calligraphic capital letters.. The bulk fields dual to these operators are the metric , the dilaton , and the axion . For example, the IRCFT energymomentum tensor can be obtained from the asymptotic expansion of the bulk metric in FeffermanGraham gauge, which takes the form
(5) 
where denotes the holographic radial coordinate, with being the location of the conformal boundary of the bulk spacetime. The tensor above is also a local functional of the boundary metric , is nontrivial when the latter is curved, and is explicitly known (see deHaro:2000xn ()). Likewise the boundary values of the axion and dilaton are and , respectively.
We also have to specify how , and are determined by the YangMills color fields as appropriate gaugeinvariant tensors. At leading order in , the most general forms of these sources are:^{3}^{3}3We also require that the full action is CPinvariant so that we can rule out  or  couplings.
(6a)  
(6b) 
where , and are dimensionless free parameters. The IRCFT is thus determined by the color fields, after assuming appropriate initial conditions and requiring absence of naked singularities in the bulk spacetime. Similarly, all other IRCFT operators are also determined by the color fields of the glasma via holographic dynamics.
Heuristically, the above form of the bulk fields at the boundary can be understood in terms of renormalisation group (RG) flow, where the scale of the flow is related to the radial direction of the dual gravity theory. Going along the radial coordinate both the sources (including the background metric) and the single trace operators of the CFT evolve in the dual geometries. It was shown in Behr:2015yna (); Behr:2015aat () that it can be recast in a precise form of RG flow in which the Ward identities of single trace operators giving local conservation laws preserve their form along the scale evolution, so that the sources become functionals of the ultraviolet degrees of freedom. Although this RG flow occurs in a fixed background metric, the sources emerge as scaledependent effective dynamical objects whose evolution is described by a dual diffeomorphisminvariant classical gravity theory in one higher dimension in the large limit. In order to include weakly coupled UV degrees of freedom which cannot be described by a dual classical gravity theory, it is natural to stop the geometric description of dynamics at a certain scale, in our case the saturation scale and assume that the effective sources and background metric at that scale are functionals of the operators of the weakly coupled UV fields instead of the UV modes of the strongly coupled holographic CFT. Therefore the boundary metric (6a) should be rather viewed as an effective metric that accounts for the marginal deformation of the IRCFT due to the coupling between the soft and hard modes at the scale . In fact, as we will show below, the full energymomentum tensor that follows from our model lives in the background metric , which is set to eventually.
The appropriate initial conditions in gravity, in the context of heavyion collisions, is that the bulk geometry is pure with vanishing dilaton and axion fields Iancu:2014ava (), reflecting the fact that the initial dynamics is primarily in the hard sector. Thus imposing the boundary values (6) on all the bulk fields and demanding regularity at the future horizon, we obtain a unique gravity solution which gives a welldefined that is equal to the dual gravitational onshell action. It has been observed in Iancu:2014ava () that the hardsoft couplings do not modify the glasma initial conditions Kovner:1995ja (); Kovner:1995ts () and this remains true in the extended construction here as well.^{4}^{4}4Technically, one may need to make the hardsoft couplings , and timedependent, e.g. proportional to , such that they start from zero and become almost a constant at a time scale of order , the time required by the uncertainty principle for a gluon of virtuality to emit a soft quanta Iancu:2014ava ().
By varying the above action (1) with respect to the YangMills fields according to
(7) 
we obtain the equations of motion for the YangMills color fields modified by the marginal operators of the IRCFT
(8) 
In order to make clear that all terms in the equations of motion indeed have the same tensor structure, it is useful to define the following new tensorial objects
(9) 
such that the modified YangMills equations read
(10) 
It is to be noted that , and are tensors living in the background metric , because is itself such a tensor and the factor is an invariant scalar under diffeomorphisms.^{5}^{5}5Indeed this factor has a nice geometric interpretation. One can readily check that if is a local conserved current in the background metric , meaning that it satisfies with being the covariant derivative constructed from , then is a conserved current in the background satisfying with being the covariant derivative constructed from . In the above equations indices are still lowered and raised with the metric and its inverse respectively, while is related to in (2) via .
The full energymomentum tensor of the coupled UVIR model is obtained by varying the action (1) with respect to the metric according to
(11)  
When the YangMills metric is finally set to the Minkowski metric , this gives
(12)  
In the following we will refer to as the energymomentum tensor describing the hard sector, while the remainder of , which is obtained from , will be ascribed to the soft sector. These latter contributions include the effects of interactions between the hard and the soft sector as apparent from the terms involving products of and expressions bilinear in . However, there is no unambiguous separation between purely soft and softhard contributions. Instead of one could equally well separate off e.g. or as putative purely soft part, which would all give slightly different decompositions into a soft energymomentum tensor and mixed terms involving also the YangMills field (except when , where the different soft energymomentum tensors coincide).^{6}^{6}6The entropy of the soft sector can however be tracked by considering the area of the black hole horizon forming in the gravitational dual. In Appendix A we explicitly show that the full energymomentum tensor is conserved on shell, i.e., if we impose the equations of motion (10) together with the Ward identity for local conservation of energy and momentum of the IRCFT in the selfconsistent background .^{7}^{7}7This Ward identity, which is a generic feature of any field theory that can be coupled to an arbitrary background metric in diffeomorphism invariant manner, also follows from the vector constraints of the dual gravitational theory.
The existence of a full energymomentum tensor which is locally conserved in the actual background metric for the YangMills dynamics, i.e. , is the primary improvement on the original semiholographic construction of Ref. Iancu:2014ava () that has been achieved here. In order to compare with Iancu:2014ava (), it is useful to define new variables:
(13) 
which transform as tensorial densities. Using these variables, we can replace the effective action (1) by
(14)  
which is invariant under diffeomorphisms. Treating , , and as independent IRCFT variables, we can vary the above action with respect to the YangMills gauge fields to obtain the equations of motion (10), while variation with respect to yields the full energymomentum tensor (12), eventually setting to the flat Minkowski space metric.
To linear order in the coupling constants (without ), to which Iancu:2014ava () had restricted itself, the modified glasma field equations of Iancu:2014ava () are reproduced by (10) apart from a factor of in the term proportional to and a factor of in the term proportional to . Beyond linear order in , the crucial difference is the presence of in the densities (2). While the entire system is residing in flat Minkowski space, the IRCFT is effectively living in a nontrivial background . Keeping all orders in is necessary to have an exactly conserved energymomentum tensor.^{8}^{8}8Although inconsequential as far as the equations of motion are concerned, for the possibility to derive the conserved total energymomentum tensor from (14) it is also important that the last term in (14) involves the trace of with respect to and not only a contraction with .
As suggested in Iancu:2014ava (), the equations of motion may be solved selfconsistently by an iterative process. First the classical YM equations with vanishing expectation values for the soft sector operators and are solved. With this solution the sources for the gravitational problem are evaluated and its field equations are solved in a second step. With the gravity solution at hand the IR operators are extracted and plugged back into (10), and the next round of the iteration process can be performed. This is done until convergence for both sectors is reached. At each step in the iteration procedure, the initial conditions in the YangMills and gravity sectors mentioned earlier are held fixed. An important feature of this approach is that the usual adhoc initial conditions used for gravity calculations to model thermalization can now entirely be determined by the associated colorglass condensate description as discussed above.
Since the initial glasma field configurations of a heavyion collisions involve strong longitudinal chromo electric and magnetic fields and thus significant Pontryagin density, it will also be of interest to study its coupling to the gravitational axion of the dual IRCFT provided by the term involving in (14). Indeed, a nontrivial axion field has been introduced previously in static models of strongly coupled anisotropic superYangMills plasma Mateos:2011ix () with interesting consequences such as a violation of the usual bound on the shear viscosity Rebhan:2011vd (). The presence of a nonvanishing Pontryagin density is moreover of central interest to anomalous transport phenomena such as the chiral magnetic effect Kharzeev:2015znc ().
3 A simple test case
In this section, we present the first numerical test of the above semiholographic setup in a very simple test case of coupling classical YangMills simulations to a holographic description of a strongly coupled soft sector. In this test case the energymomentum tensor is homogeneous and isotropic, but both the UV and IR degrees of freedom have nontrivial (0+1dimensional) dynamics. This allows us to check for convergence of the proposed iterative scheme for solving both the UV and IR dynamics. Furthermore, we also check that, when the iterative procedure converges, the full energymomentum tensor (12) of the combined system is indeed conserved.
For simplicity, we also switch off the hardsoft couplings and so that the dilaton and the axion are not excited, while retaining . The full solution in our test case shows periodic transfers of energy from hard to soft sector and vice versa without any thermalization due to the fact that the symmetries in the gravitational sector of the test case exclude any propagating degrees of freedom and thus do not allow for dynamical black hole formation or perturbation. Thus no energy is deposited irreversibly in the thermal part of the soft sector. As shown below the hard sector only changes the way of how a preexisting black hole is perceived at the boundary. Nevertheless, this amounts to a nontrivial backreaction on the hard sector.
Moreover, since the simple situation presented below lies at the basis of the more complicated scenarios we want to address in the future, it is essential to study and to fully understand the dynamics of our test case.
3.1 UV sector: Classical dynamics of homogeneous YangMills fields
The simplest configurations of the glasma, described by classical YangMills equations, are produced by homogeneous color gauge fields. For simplicity, we shall consider SU(2) YangMills theory. Using temporal gauge , with , the YangMills equations of spatially homogeneous fields are a set of 9 coupled nonlinear ODE’s. Setting , they are given by
(15) 
which immediately follows from , , and .
In temporal gauge, Gauss’ law, , has to be imposed as a constraint. In the homogeneous case it reduces to
(16) 
which is easy to satisfy by initial conditions where either or is set to zero.
The resulting dynamics of the 9 degrees of freedom is in general completely chaotic. The resulting energymomentum tensor contains a conserved positive energy density, vanishing Poynting vector , but the spatial stress tensor components (diagonal and nondiagonal) fluctuate with the only constraint of 4dimensional tracelessness.
The energymomentum tensor can be made diagonal by locking color and spatial indices, i.e. assuming , which reduces the number of degrees of freedom from 9 to 3. Switching on the semiholographic coupling in (14) still allows us to restrict to a diagonal tensor , which gives extra source terms to the equations of motion (15) that can be obtained explicitly from (10), but as can be explicitly checked the Gausslaw constraint (16) also remains unchanged.
The simplest nontrivial case is obtained by additionally requiring isotropy of the stress tensor. Homogeneity and spherical symmetry with the same pressure in all three directions from fields with nontrivial time dependence can be obtained by setting . Then the color electric fields are
(17) 
forming a single anharmonic oscillator with
(18) 
The expressions for the preserved energy and pressure read
(19) 
The equation of the anharmonic oscillator (18) has a closedform solution in terms of the Jacobi elliptic function
(20) 
which is a double periodic function in the complex plane. Along the real axis one has sinusoidal oscillations with the peculiarity that around a zero there is a linear term but no cubic term because the potential is flat at the origin, .
In the left panel of Fig. 1 the colorelectric and colormagnetic fields are shown for initial conditions corresponding to and in (20). ( is chosen such as to match the numerical solutions of Fig. 3 in units where and in the limit that the entire energy is in the YangMills fields.) The right panel shows the conserved energy density and the oscillating quantities and . The negative action density is seen to oscillate between and without having a mean value of zero; the topological charge density has the same extremal values with a more complicated but symmetric oscillation pattern.
When coupled to the IRCFT, the energymomentum tensor of the YangMills theory is no longer conserved separately. In order to use the above ansatz in a semiholographic setup in the simplest way, we want to find an appropriate exact gravity solution that allows for a time dependent boundary metric of the form (6a).
3.2 IRCFT sector: Analytic gravity solution
The simplest IRCFT configuration that we can couple selfconsistently to the classical YangMills system considered above is one that retains the same symmetries, namely homogeneity and isotropy. A remarkable simplification happens when we consider the case in which and in (6) vanish. The only nontrivial marginal deformation of the IRCFT in this case is via the background metric (that is identified with the boundary metric of the dual gravity solution), which takes the form:
(21) 
Note that in order to preserve the signature and regularity of the background metric the coupling must lie in the interval:
(22) 
A crucial simplification for the following calculation is that the metric (21) is conformally flat.
As mentioned above, we impose homogeneity and isotropy on the IRCFT energymomentum tensor . When the IRCFT is holographic, it follows that the dual geometry should also have homogeneity and isotropy, since both the data, namely the boundary metric and , which determine the solution, have these properties. Furthermore, as the hardsoft couplings and are switched off, the bulk dilaton and axion fields vanish. This allows us to apply Birkhoff’s theorem, according to which the bulk metric should be locally diffeomorphic to the standard AdSSchwarzschild black brane solution:
(23) 
where is related to the mass of the black brane. In our case, will be a free parameter related to the IRCFT initial conditions (particularly the initial energy in this sector).
The IRCFT state dual to the AdSSchwarzschild black brane (23) is the thermal state (with the temperature determined by the mass parameter ) living in flat Minkowski space, which is the boundary metric of this gravity solution. Since we are interested in a homogeneous and isotropic IRCFT state that lives in the metric (21), we should apply a bulk diffeomorphism which is nontrivial at the boundary and is such that the boundary metric transforms from to (21). At the boundary, this bulk diffeomorphism should reduce to a precise combination of a Weyl transformation and a diffeomorphism of the time coordinate, since (21) is conformally flat. Indeed, such a bulk diffeomorphism is unique (once we also choose the final gauge), and is explicitly given in Appendix B. In Appendix B we also calculate the canonical charge of the bulk space time showing that up to anomalous effects the total gravitational energy is constant and equals that of the AdSSchwarzschild black hole with a flat boundary. Applying this bulk diffeomorphism, we obtain our desired gravity solution from which we can obtain defined in (9) in the dual IRCFT state, through the standard holographic dictionary that states:
(24) 
where denotes the holographically renormalized onshell fivedimensional EinsteinHilbert action. Since in (21) is conformally flat, the energymomentum tensor is not renormalizationscheme dependent.^{9}^{9}9Scheme dependence arises from the possibility of adding a covariantly conserved traceless tensor with the correct conformal weight to that is a local functional of the boundary metric (note that evaluated in the background metric is scheme independent). In 4 dimensions this schemedependent contribution is proportional to the Bach tensor which vanishes on Weylflat (i.e. conformally flat) backgrounds.
At this stage, it is interesting to note that we can also derive the form of the required homogeneous and isotropic in the IRCFT via a general alternative method, which works also when the IRCFT is not holographic. We still need to assume that, except for a nontrivial background metric, all other background sources vanish, which requires us to put the couplings and to zero. The only additional assumption that we need to put in is that the IRCFT state is the (timedependent) conformal (plus a coordinate) transformation of the thermal state (with an arbitrary temperature), where the transformation brings to the desired background metric (21) determined by the classical YangMills fields. Since we cannot take the benefit of Birkhoff’s theorem that applies on the gravity side in the large limit in holographic CFTs, we cannot say that this should be the unique homogeneous and isotropic IRCFT living in this background metric. Nevertheless,
we can selfconsistently assume that the IRCFT state is the conformally transformed thermal state.
Under conformal transformation, transforms as a contravariant tensor of rank two and with Weyl weight two in a CFT, up to a stateindependent and renormalizationscheme independent anomalous term. In a 4D CFT, this anomalous term in a conformally flat background metric is given by (see for example PhysRevD.16.1712 (); Herzog:2013ed ()):
(25) 
where is the central charge associated with the Euler density.^{10}^{10}10The central charge associated with the Weyltensorsquared term does not contribute here in a conformally flat background metric. As this anomalous piece is stateindependent, we can obtain this from the vacuum in a conformally flat background metric. Thus, we need to add the above anomalous piece (evaluated in the metric (21) to the covariant piece obtained after conformal transformation to compute the desired IRCFT . In a holographic CFT, as expected on general grounds, we get the same result in this method as obtained via the direct application of the holographic dictionary on the dual gravity solution as mentioned before, by using
(26) 
The above is a universal result for a strongly coupled large holographic CFT.
Either by using the standard holographic dictionary (for details see Appendix B) or via the simplified procedure mentioned above, we obtain the (diagonal) components of as follows:
with
(28) 
The terms proportional to are simply the result of the transformation of the energymomentum tensor density of the AdSSchwarzschild spacetime with flat boundary conditions and thus only involve the YangMills pressure without derivatives. This part of the energymomentum tensor is still traceless and (covariantly) conserved on its own with respect to the metric . Furthermore, it is also the most relevant contribution to the energymomentum density in a small expansion which reads
(29)  
(30) 
As we shall see below, only the combination contributes in the equations of motion of the semiholographic model. Therefore the leadingorder effect of the backreaction on the YangMills fields, mediated by the deformation of the IRCFT due to the YangMills fields which determine , is of order . To leading order , the IRCFT acts on the YangMills fields through the soft thermal bath that one starts with by choosing .
The terms independent of in Eq. (3.2) are due to the nonvanishing Ricci tensor of and their trace gives the conformal anomaly, which in our case is determined solely by the Eulerdensity associated with . These only contribute at nonstationary points of the YangMills pressure, i.e., for , and are of order .
3.3 Coupling the UV with the IR sector
We now have all the ingredients at hand to test our modified semiholography proposal. The equations of motion (10) for the coupled system with a homogeneous and isotropic ansatz for the UVYangMills gauge fields (17) coupled to a homogeneous and isotropic IR energymomentum tensor become
(31) 
where and are given by (3.2). It is remarkable that only the combination is needed, which is given in closed form by
(32)  
where we introduced the abbreviation .
The full energy density for our test case is obtained by taking the zeroth component of the energymomentum tensor (12), which can be expressed in the following convenient form:
(33) 
In order to solve (31), which is an ordinary fourthorder differential equation when in is expressed in terms of through (19), we will use the iterative algorithm proposed in Iancu:2014ava () and test its usability. By interpreting as a fixed external source, which is updated after each iteration, this reduces to a secondorder differential equation for . While in principle this method should not be necessary for our test case, in practice we have not been able to find regular solutions of the above highly nonlinear fourthorder equation other than by following the iterative procedure. Moreover, one has to keep in mind that for more complicated dynamics, e.g., for an anisotropic situation or for , the expression of in terms of the YangMills fields (here ) will not be explicitly known.
Eq. (31) is reminiscent of an equation of motion for an anharmonic oscillator where the coefficient of the term determines the frequency of the oscillations, whereas the last term acts as (anti)damping term. In order to obtain regular oscillating solutions the frequencies are constrained to take real values.
Before discussing the full numerical result, we describe the first two steps of the algorithm, allowing us to extract analytic behavior which approximates the full solution very well for sufficiently small values of . In the first step we set which amounts to the solution for we have already discussed in section 3.1 and for which . Inserting the latter into (32), the updated source now reads
(34) 
which is larger than irrespective of the sign of .
For a special choice of initial conditions, either , or , , it follows automatically that at the initial time always takes the value given in (34).^{11}^{11}11The case , implies while in the case , one has and hence one obtains from the equations of motion.
In the second step of the iterative process the derivative of still vanishes and we only have to solve the second order differential equation
(35) 
Choosing the initial conditions and , again an analytic solution in terms of Jacobi elliptic functions can be found,
(36) 
where denotes the complete elliptic integral of the first kind, which is the quarter period of the Jacobi elliptic function, e.g. . Accordingly we may call the frequency of the anharmonic oscillations. As already mentioned, demanding a regular solution imposes a reality condition on , which in turn puts bounds to the value of in addition to those put on guaranteeing regularity of . The allowed parameter space is illustrated in Fig. 2. The total initial energy of the full semiholographic system for this choice of initial conditions is given by
(37) 
which remains true to all orders of the iterative algorithm.
Starting with the third step of the iterative algorithm requires to solve the second order equation for numerically. Note that for positive we find , while for negative we find , meaning that for negative the allowed region for the values of is further restricted in order to ensure regularity of the metric as shown by the blue line in Fig. 2. There we also show lines of constant values of that completely fit within the restricted regions. For positive we find and for negative this condition amounts to .
In Fig. 3 we present the numerical solution for three different choices of with and constant energy : , , . These choices are depicted by the colored markers in Fig. 2.
In the upper panel of Fig. 3, the blue horizontal line marks the total energy density, and the three oscillating lines give the YangMills part of it for the three choices of . The difference to the total energy density is the oppositely oscillating component contained in the soft modes together with their interaction energy with the hard modes.^{12}^{12}12Although the entropy of the dual black hole and its intrinsic temperature is unchanging, the changing boundary metric leads to a changing energy density contribution in (12), as further discussed in Appendix B. However, as we discussed above, there is no unambiguous separation of purely soft contributions from the explicit softhard interaction terms in the full energymomentum tensor (12). E.g., rewriting everything in terms of instead of would suggest a different split of the contributions coming from into soft and softhard parts, again with both changing in time. From the constancy of the entropy of the black hole one can however conclude that there is no change in the thermalized part of the energy in the soft sector.
Fixing the energy density in (37) and varying for the three solutions means that we have to adjust the parameter , which is related to the black holes mass, accordingly. Going from higher to lower values in with fixed means that is increased and the black hole made larger. (The case corresponds to the trivial solution where one has exactly .) In a more realistic setup where the gravity solution is dynamical and not just a gauge transformation of the AdSSchwarzschild black hole, we expect that due to the interaction between the hard and soft sector the growing black hole draws energy from the hard modes as the system thermalizes. The UV energy density thus may shrink and get deposited in the IRsector. This is mimicked here by choosing different initial conditions. Interestingly, with the choice of positive in the example shown in Fig. 3, the wavelength of the oscillation increases as the YangMills energy density decreases, which is not the case for negative . Furthermore, for positive the trace term depicted in the lower panel of Fig. 3 is always positive, consistent with lattice results of QCD thermodynamics Boyd:1996bx (); Borsanyi:2010cj (), where is often called the “interaction measure”.
We applied two criteria in order to decide whether the algorithm converges. The first is of course to check whether equation (31) evaluated at the solution for is satisfied sufficiently, which is nontrivial, since the solution for was obtained for source terms evaluated with the solution of the previous iteration step. The second criterion is that the total energy evaluated at the solution for is sufficiently close to the value prescribed in Eq. (37) respectively. In the solution presented in Fig. 3 both criteria were satisfied up to order which is smaller than any term appearing in (31) in particular the one involving the fourth order derivative of .
Figure 4 shows the convergence of the iterative solution for the case (b). From the fourth iteration onwards, there is no visible change of the numerical result.
4 Conclusions
In this paper we presented an improved and extended version of the semiholographic model proposed in Iancu:2014ava (). The idea behind semiholography is to construct a phenomenological model for heavyion collisions that is able to incorporate the interaction between the weakly coupled UV and the strongly coupled IRsector. This is done by assuming that the UV sector is given by overoccupied gluon modes admitting a description in terms of classical YangMills fields, while the strongly coupled IRsector is described by a conformal field theory with a holographic dual.
We presented a new action where such a mechanism can be implemented, and we constructed the full energymomentum tensor of the coupled theory which is locally conserved and thus can track the energy transfer between the two sectors. The full energymomentum tensor consists of the standard YangMills theory expression plus contributions derived from the effective action of the conformal field theory which is deformed by the marginal operators of the YangMills theory. The latter contributions thus comprise both purely soft and softhard ones, which however cannot be disentangled unambiguously; only the thermal part of the soft sector has a welldefined meaning in terms of the black hole horizon of the holographic gravity dual.
Moreover, we have presented first numerical tests of the iterative procedure proposed for solving the evolution of the semiholographic model. By assuming homogeneity and isotropy we were able to construct a simple test case with closed analytic solutions for the two decoupled sectors. Coupling them together via the tensorial coupling only, we numerically solved for the evolution of the fields and observed quick convergence of the algorithm and observed energy exchange between the YangMills part and the conformal field theory with constant total energy. This is already a nontrivial result and is a proof of principle of this semiholography proposal.
Of course, due to the simplicity and high symmetry of this test case we could not observe thermalization. This was expected because without any propagating degrees of freedom our gravity solution does not incorporate dynamical black hole formation, only timedependent diffeomorphisms of a preexisting black hole, i.e., the black hole temperature and the entropy measured by the surface gravity and the horizon area respectively are not altered. In order for the system to relax, more degrees of freedom must be included. This can be done by introducing anisotropy in the spacetime along the lines of Chesler:2008hg () and also making the YangMills fields anisotropic. It is then expected that the black hole is able to draw energy from the hard modes and that isotropization occurs. Another possibility is to stay isotropic and to turn on one or both of the scalar fields on the gravity side coupled to the Lagrange density and the Pontryagin density on the field theory side, respectively. The latter would be particularly interesting in view of anomalous transport phenomena such as the chiral magnetic effect Kharzeev:2015znc () and also with regard to the results of Ref. Rebhan:2011vd () on the shear viscosity in strongly coupled anisotropic systems. We plan to tackle these more complicated scenarios in future work.
Depending on the initial conditions and/or the values of , and , various different scenarios of thermalization may appear, e.g., the hard modes may eventually drain their energy almost completely to the black hole, or the hard modes might retain a significant fraction of their energy even at late time, while the full energymomentum tensor (12) approaches a diagonal form. In the latter case, we would expect that the effective hydrodynamic description which results from the fluid/gravity correspondence Rangamani:2009xk () will not suffice to describe the late stage of the evolution prior to hadronization. Since at late times, where the relatively hard gluons are less densely populated, a kinetic theory approach may be more suitable than the classical field theory (glasma) description, it would also be interesting to understand how to couple kinetic theory to a holographic CFT in our semiholographic framework. In this context, it may be useful to follow Muller:2015maa (); Yang:2015bva (), where a similar attempt has been made in context of constructing a kinetic theory of leptons and photons when the latter are interacting with strongly coupled QCD matter. This could e.g. have an important bearing on the photon puzzle Adare:2011zr (); Lohner:2012ct () that pertains to the late stage of the evolution.
In the future, we may also hope to determine the (so far free) hardsoft coupling constants , , and in terms of to a certain degree of approximation, by using renormalisation group techniques as discussed in Behr:2015yna (); Behr:2015aat (). In this case, the semiholographic model could eventually lead to sharp predictions.
Acknowledgments
We thank C. Ecker, N. Gaddam, E. Iancu, and D.L. Yang for useful discussions. A. Mukhopadhyay acknowledges support from a Lise Meitner fellowship of the Austrian Science Fund (FWF), project no. M1893N27; F. Preis and S. Stricker were supported by the FWF project P26328N27.
Appendix A Conservation of the full energymomentum tensor
In this Appendix we show that the full energymomentum tensor
(38)  