PRODUCTION OF THERMAL PHOTONS IN A SIMPLE CHIRAL-HYDRODYNAMIC MODEL

Production of thermal photons in a simple chiral-hydrodynamic model

Abstract

We use a self-consistent chiral-hydrodynamic formalism which combines the linear model with second-order hydrodynamics in dimensions to compute the spectrum of thermal photons produced in Au+Au collisions at GeV. The temperature-dependent shear viscosity of the model, , is calculated from the linearized Boltzmann equation. We compare the results obtained in the chiral-hydrodynamic model to those obtained in the second-order theory with a Lattice QCD equation of state and a temperature-independent value of . We find that the thermal photon production is significantly larger in the latter model due to a slower evolution and larger dissipative effects.

Thermal photons, heavy ion collisions, viscous fluid dynamics
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PACS numbers: 25.75.-q, 24.10.Nz, 24.85.+p

1 Introduction

In this paper we focus on the spectrum of thermal photons produced during the expansion of the fireball created in Au+Au collisions at GeV. Photons created in the interior of the fireball pass through it without any interaction, thus giving information on the properties of bulk nuclear matter [1, 2, 3, 4, 5, 6]. Thermal photon spectra have been calculated within the framework of different fluid dynamics models [1, 6, 5, 3, 4] as well as a hybrid kinetic-hydrodynamic model [7]. Here we employ a self-consistent chiral-hydrodynamic model combining second-order (SOT) hydrodynamics and the linear model (LSM), in which the temperature-dependent is computed from kinetic theory [8]. We compare the spectrum of thermal photons with that obtained from the same SOT with a Lattice QCD-inspired equation of state (EOS) and a temperature-independent value of . The latter model is commonly employed in the study of hadronic observables of heavy ion collisions. The purpose of this contribution is to quantify the differences in thermal photon spectra that arise from differences in these two fluid dynamical models when they are taken as a whole. In other words, no attempt is made to disentangle the impact of EOS or the temperature dependence of on the thermal photon spectra (see [4] for a study along this line).

2 Chiral-hydrodynamic model

We now describe the coupling between the chiral fields and the quark fluid, the latter described by second order boost invariant fluid dynamics (see [3, 4, 8] for further details).

The classical equations of motion of the LSM are given by

(1)

where and

(2)

is the Fermi–Dirac function and is the potential exhibiting chiral symmetry breaking. These are solved selfconsistently together with the conservation equations for the combined system of chiral fields plus quark fluid

(3)

where , is the comoving time derivative, is the spatial gradient, and is shear tensor. The evolution equation for contains terms up to second order in velocity gradients and it is given in [3, 4]. In order to estimate the temperature dependence of the shear viscosity in the LSM, we adapt the method described in [9] and employ the linearized Boltzmann equation in the relaxation time approximation (see [8]).

To compute the spectrum of thermal photons created during the evolution of the fireball we consider the processes of Compton scattering, annihilation and bremsstrahlung in the QGP phase, and , and in the hadron phase [1], as described in [3]. In all cases, the nonequilibrium distribution function of the quarks, , is calculated from Grad’s ansatz.

3 Results

We now go over to present our results. As a typical example of a conformal fluid we take and corresponding to the supersymmetric Super–Yang–Mills plasma. We use a 13 fm 13 fm transverse plane, and set the impact parameter to fm. The initialization time is set to fm/c, and we use and as initial values. The initial energy density profile is obtained from Glauber’s model, with a temperature MeV at the center of the fireball. We take and with fm as initial values for the chiral fields. We use the isothermal Cooper-Frye freeze–out prescription with a freeze-out temperature MeV. The critical temperature is set to MeV.

The upper panel of Figure 1 shows the square of the speed of sound corresponding to the LSM with , which yields a smooth crossover, and to the EOS calculated by Laine and Schröder [13] which connects a high-order weak-coupling perturbative QCD calculation at high temperatures to a hadron resonance gas at low temperatures via an analytic crossover. Recent works have shown that the comparison of hydrodynamic simulations with RHIC data favor a smooth crossover over a first-order transition [14], and this is the reason for considering a crossover (and not a first-order phase transition) in the LSM. There is no appreciable change in the photon spectrum provided , but if or the dip in at becomes too sharp or fades away, respectively, resulting in a temperature dependence that strongly disagrees with the one obtained in Lattice QCD calculations. As it can be seen from Figure 1, for large temperatures the conformal limit is reached, while for low values goes to zero. Note also that the transition region is significantly broader in the LQCD EOS than in the LSM.

Figure 1: (Color online) Speed of sound of the LSM and that of the model EOS of Laine and Schröder (upper panel); in the LSM (lower panel). The value of the coupling constant is .

The lower panel of Figure 1 shows as a function of temperature for the LSM with . It is seen that the ratio remains small () in the QGP phase and starts increasing abruptely for . For this reason we must impose a cut-off in the value of ; we take 1 . For the SOT with the LQCD EOS we consider a temperature-independent value , which corresponds to the averaged value throughout the evolution.

Figure 2 shows the different contributions to the total thermal photon spectrum coming from the QGP and the hadronic phases, for the LSM and the SOT with the Lattice QCD EOS.

Figure 2: (Color online) Contributions to the thermal photon spectra from the QGP and hadronic phases for the LSM with and the SOT with Lattice QCD EOS.

It is seen that in all cases the photon spectrum is considerably smaller in the LSM, the difference being larger in the hadronic phase. The difference between the spectra in both models is practically independent of , except at very low values where the difference becomes slightly larger. In both models, the contribution of the hadronic phase to the photon spectrum is dominant over that coming from the QGP phase.

There are two reasons that make the spectrum obtained from the chiral model smaller than the corresponding to the Lattice QCD EOS. First, the hydrodynamic evolution is much faster in the LSM model, essentially because the speed of sound is on average larger than the one corresponding to the Lattice QCD EOS. This is illustrated by the fact that the freeze-out temperature is reached in fm/c in the LSM and in fm/c, which represents a significant difference. The other reason is that the shear tensor is on average significantly smaller in the LSM, leading to a smaller contribution of dissipative effects to the total photon spectrum.

4 Conclusions

Using a simple self-consistent chiral-hydrodynamic model based on the linear model and conformal second-order hydrodynamics, we calculated the spectrum of thermal photons including nonequilibrium corrections produced during the evolution of the fireball created in Au+Au ultrarelativistic collisions. Compared to the results obtained with a commonly used second-order fluid dynamic model with an equation of state inspired in Lattice QCD and a temperature independent , we find that the photon production is significantly smaller in the chiral-hydrodynamic model, due to a faster evolution and to smaller dissipative corrections to the nonequilibrium distribution function.

Acknowledgements

The authors acknowledge FAPESP (São Paulo, Brazil) for financial support.

Footnotes

  1. Any hydrodynamic theory necessarily breaks down when viscosity is large enough. The value of at which it is sensible to impose this cut-off can be estimated in (see e.g. [8]).

References

  1. T. Peitzmann and M. H. Thoma, Phys. Rep. 364, 175 (2002).
  2. A. Adare et al. (PHENIX Collaboration), Phys. Rev. Lett. 104, 132301 (2010).
  3. J. Peralta-Ramos and M. S. Nakwacki, Nucl. Phys. A 851, 44 (2011).
  4. J. Peralta-Ramos and M. S. Nakwacki, Mod. Phys. Lett. A 27, 1250050 (2012).
  5. J. R. Bhatt et al, arXiv:1005.2756 [hep-ph]; ibid, JHEP 11, 106 (2010).
  6. K. Dusling, Nucl. Phys. A 839, 70 (2010).
  7. B. Baeuchle and M. Bleicher, Phys. Rev. C 82, 064901 (2010); ibid, Phys. Lett. B 695, 489 (2011); ibid, Phys. Rev. C 81, 044904 (2010).
  8. J. Peralta-Ramos and G. Krein, Phys. Rev. C 84, 044904 (2011).
  9. C. Sasaki and K. Redlich, Nucl. Phys. A 832, 62 (2010); ibid. Phys. Rev. C 79, 055207 (2009).
  10. C. T. Traxler and M. H. Thoma, Phys. Rev. C 53, 1348 (1996).
  11. P. Aurenche et al, Phys. Rev. D 58, 085003 (1998).
  12. F.D. Steffen and M.H. Thoma, Phys. Lett. B 510, 98 (2001); H. Nadeau et al, Phys. Rev. C 45 3034 (1992).
  13. M. Laine and Y. Schröder, Phys. Rev. D 73, 085009 (2006).
  14. S. Pratt, Phys. Rev. Lett. 102, 232301 (2009); W. Florkowski, Nucl. Phys. A 853, 173 (2011).
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