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Thermal photons in A+A collisions at RHIC energies D.Peressounko RRC “Kurchatov Institute”

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Presentation on theme: "Thermal photons in A+A collisions at RHIC energies D.Peressounko RRC “Kurchatov Institute”"— Presentation transcript:

1 Thermal photons in A+A collisions at RHIC energies D.Peressounko RRC “Kurchatov Institute”

2 2005 RHIC & AGS Annual User’s meeting D.Peressounko, RRC “Kurchatov Institute”2 How to calculate thermal photon yield Pre-equilibrium contribution: Neglect it; Use cascade models; Model with hydro. d3Nd3N dy d 2 P t = ∫ R(T,  u) d 4 x Key features of calculations: Emission rates for QGP and RHG Dynamic model: Fireball; 2+1 Bjorken hydrodynamics; 3+1 hydro; Initial conditions:  0 (  0 or T 0 ) EoS  R – emission rate from the unit 4-volume at a temperature T(x) and chemical potential  (x), boosted with 4-velocity u(x);  – space-time volume, occupied by the system.

3 2005 RHIC & AGS Annual User’s meeting D.Peressounko, RRC “Kurchatov Institute”3 Thermal photon emission rate from QGP Compton and annihilation (qg→q ,qq→g  ) processes in HTL framework J.I. Kapusta, P. Lichard, D. Seibert, Phys. Rev. D44, 2774 (1991); Erratum, ibid D47, 4171 (1993). R. Baier, H. Nakkagawa, A. Niegawa, K. Redlich, Z. Phys. C53, 433 (1992). Annihilation with rescattering and bremsstrahlung P. Aurenche, F. Gelis, R. Kobes, E. Petitgirard, Z. Phys. C75, 315 (1997). P. Aurenche, F. Gelis, R. Kobes, H. Zaraket, Phys. Rev D58, 085003 (1998). P. Aurenche, F. Gelis, H. Zaraket, JHEP 0205, 043 (2002). P. Aurenche, F. Gelis, H. Zaraket, Phys. Rev. D62, 096012 (2000). Inclusion of the LPM effect P. Arnold, G.D. Moore, L.G. Yaffe, JHEP 0111, 057 (2001). P. Arnold, G.D. Moore, L.G. Yaffe, JHEP 0112, 009 (2001). P. Arnold, G.D. Moore, L.G. Yaffe, JHEP 0206, 030 (2002). Complete calculations in  and  s

4 2005 RHIC & AGS Annual User’s meeting D.Peressounko, RRC “Kurchatov Institute”4 Thermal photon emission rate from hadron gas Photon emission in reactions in  gas J. I. Kapusta, P. Lichard, and D. Seibert, Phys. Rev.D 44, 2774 (1991); Added a 1 as a intermediate state in  → a 1 →  L. Xiong, E. V. Shuryak, and G.E. Brown, Phys. Rev.D 46, 3798 (1992). Consistent treatment of contribution of a 1 resonance C. Song, Phys. Rev. C 47, 2861 (1993). Exploring effects of hadron mass modifications in hot matter P. Ko and S. Rudaz, Phys. Rev. D 50, 6877(1996). J.K. Kim, P. Ko, K. Y. Lee and S. Rudaz, Phys. Rev.D 53, 4787(1996). S. Sarkar, J. Alam, P. Roy, A. K.Dutt-Mazumder, B. Dutta-Roy and B. Sinha, Nucl. Phys. A 634, 206 (1998); P. Roy, S. Sarkar, J. Alam and B. Sinha, Nucl. Phys. A 653, 277 (1999). Y. C. Shin, M. K. Cheoun, K. S. Kim and T. K. Choi, Eur. Phys. J. A 14, 87 (2002). Inclusion of the contribution of strange mesons,  in t-channel and baryons S. Turbide, R. Rapp and C. Gale, hep-ph/0308085. Jan-e Alam, Pradip Roy and Sourav Sarkar, hep-ph/0310168 Extensive set of reactions involving a 1,K,N

5 2005 RHIC & AGS Annual User’s meeting D.Peressounko, RRC “Kurchatov Institute”5 Calcutta group J. e. Alam, S. Sarkar, T. Hatsuda, T. K. Nayak and B. Sinha, Phys. Rev. C 63 (2001) 021901. QGP emission rate: Two loop, no LPM effect HG emission rate:  a 1 within different models Model: 2+1 Bjorken hydrodynamics In. Cond: T i = 265 MeV,  i =1 fm/c EoS: Bag model (  a 1,N in HG ) Evolution is not fitted neither to hadron multiplicity nor to hadron spectra.

6 2005 RHIC & AGS Annual User’s meeting D.Peressounko, RRC “Kurchatov Institute”6 D.K.Srivastava D. K. Srivastava, Pramana 57 (2001) 235. QGP emission rate: Two loop, no LPM effect HG emission rate: emission from ,a 1 gas Model: 2+1 Bjorken hydrodynamics In. Cond: T i = 670-390 MeV,  i = 0.2-1 fm/c EoS: Bag model (  a 1,N in HG )

7 2005 RHIC & AGS Annual User’s meeting D.Peressounko, RRC “Kurchatov Institute”7 Montreal group S.Turbide, R.Rapp and C.Gale, Phys. Rev. C 69, 014903 (2004). QGP emission rate: two loop with LPM effect HG emission rate: emission from  a 1,K,N gas Model: Fireball model with fixed longitudinal and transverse accelerations. In.Cond.: T i ~370 MeV   i =0.3 fm/c

8 2005 RHIC & AGS Annual User’s meeting D.Peressounko, RRC “Kurchatov Institute”8 Jyvaskyla group S.S.Rasanen, Nucl.Phys.A 715 (2003) 717. F.Gelis, H.Niemi, P.V.Ruuskanen, S.S.Rasanen, J.Phys.G30:S1031-S1036,2004 QGP emission rate: two loop with LPM effect HG emission rate: emission from ,a 1 gas Model: 2+1 Bjorken hydrodynamics In. Cond: T i = 580 MeV,  i =0.17 fm/c EoS: Bag model (rich hadronic gas) Evolution fit to reproduce hadron spectra

9 2005 RHIC & AGS Annual User’s meeting D.Peressounko, RRC “Kurchatov Institute”9 BNL-Moscow group D.d'Enterria and D.Peressounko, nucl-th/0503054 QGP emission rate: two-loop with LPM effect HG emission rate: emission from a 1,K,N gas Model: 2+1 Bjorken hydrodynamics; In.Cond:  i =0.15 fm/c; T i =610 MeV EoS: Bag model (~400 species in HG) Evolution is fit to ,K,p spectra

10 2005 RHIC & AGS Annual User’s meeting D.Peressounko, RRC “Kurchatov Institute”10 BNL-Moscow group D.d'Enterria and D.Peressounko, nucl-th/0503054 pQCD: L.E. Gordon and W. Vogelsang, Phys. Rev. D 48 (1993) 3136; Phys. Rev. D 50 (1994) 1901. PHENIX data: S.S.Adler et al., Phys. Rev. Lett. 94, 232301 (2005)

11 2005 RHIC & AGS Annual User’s meeting D.Peressounko, RRC “Kurchatov Institute”11 Comparison of predictions to PHENIX data Calculations with similar initial time (temperature) result in similar spectra. Dependence on used emission rates and details of description of evolution is modest. All calculations predict considerable thermal contribution below 3 GeV All calculations agree with data within errors.

12 2005 RHIC & AGS Annual User’s meeting D.Peressounko, RRC “Kurchatov Institute”12 What is next? Calculate centrality dependence of the thermal photon spectrum: Exploring dependence on the initial energy density. Since thermal photons reflect temperature in the medium, can we extract this temperature directly by measuring slope? Can we extract the number of effective degrees of freedom in hot matter by comparing thermal photon slope and entropy or energy density? Can we go further?

13 2005 RHIC & AGS Annual User’s meeting D.Peressounko, RRC “Kurchatov Institute”13 Correlation between apparent and initial temperature EoS with phase transition EoS without phase transition Smearing of effective temperature: Final thickness of matter Temperature gradients T(r) Collective velocity Does correlation survive? D.d'Enterria and D.Peressounko, nucl-th/0503054

14 2005 RHIC & AGS Annual User’s meeting D.Peressounko, RRC “Kurchatov Institute”14 Correlation between apparent temperature and dN ch /d EoS with phase transition EoS without phase transition Au+Au, 200 AGeV D.d'Enterria and D.Peressounko, nucl-th/0503054

15 2005 RHIC & AGS Annual User’s meeting D.Peressounko, RRC “Kurchatov Institute”15 Correlation between apparent temperature and dN ch /d Au+Au, 62 AGeV  i =4R/= 0.45 fm/c D.d'Enterria and D.Peressounko, nucl-th/0503054

16 2005 RHIC & AGS Annual User’s meeting D.Peressounko, RRC “Kurchatov Institute”16 Conclusions  At top RHIC energy thermal photons contribute to direct photon spectrum at P t <3 GeV: more precise data are necessary to make any conclusion.  Thermal photon spectrum depends mainly on initial temperature and in much smaller extend on details of evolution and emission rates.  Correlation between apparent temperature of thermal photons and maximal initial temperature in the collision is not destroyed by evolution: maximal temperature can be extracted just by measuring inverse slope at as high P t as possible.  One can directly explore phase transition by confronting apparent slope of thermal photons and charged hadron multiplicity.

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