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frm Dubna synchrophasotron

Correlation femtoscopy. frm Dubna synchrophasotron. to CERN LHC. Jan Pluta, Warsaw University of Technology. The pre-femtoscopy period. 1960. 1967. 1969. The begin of femtoscopy. 1972 ~ 4 Kopylov and Podgoretsky settled the basics of correlation femtoscopy:

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frm Dubna synchrophasotron

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  1. Correlation femtoscopy frm Dubna synchrophasotron to CERN LHC Jan Pluta, Warsaw University of Technology

  2. Thepre-femtoscopy period

  3. 1960

  4. 1967

  5. 1969

  6. Thebegin of femtoscopy

  7. 1972 ~ 4 • Kopylov and Podgoretsky settled the basics of correlation femtoscopy: • correlation function, • mixing technique, • role of space-time characteristics etc. Podgorecki, Kopylov, Smorodinski Dubna, 1974

  8. 1970

  9. 1973

  10. 1974 Correlation function Space Time

  11. Mixing technique 1974

  12. 1975 ~1990 -Grishin, propane bubble chamber group and others in Dubna - measured two-particle correlations for various reactions and two-particle systems in the energy domain of several GeV/nucleon V.G. Grishin M.I. Podgoretski Weekly meeting of propane bubble chamber group.

  13. N. Angelov et al. Two-particle correlations of secondary protons in pi-12C interactions at 40 GeV/c

  14. Momentum dependence

  15. G.N. Agakishiev et al. Dimensions of the secondary pion emission region in multi-nucleon collisions of nuclear projectiles D,He,and C with C and Ta nuclei at the incident momentum of 4.2 Gev/c per nucleon, Sov. Journ. Of Nucl. Phys, 39 (1984) 543 The first attempt to „participant dependence”

  16. First correlation function for two neutral pions

  17. 1981 Lednicky and Lyuboshitz solved the problem of final state interaction 1981 R. Lednicky and V.L. Lyuboshitz Influence of Final-stateinteraction on thecorrelatins of twoparticles withnearlyequalmomenta Dubna report: E2-81-453 Sov. Journ. Nucl. Phys. 35 (1982) 770

  18. J. Bartke, Size of the pion emission region in collisions of relativistic nuclei from intensity interferometry, Phys. Lett B (1986) 32 Summary (and the END) of static source period

  19. Q G P

  20. NA35 1988 mid-rapidity

  21. NA35 1988

  22. 1988 - Seminar of Yu.Sinyukov in Dubna

  23. Yu. M Sinyukov, Hanbury-Brown/Twiss correlations for expanding hadron and quark-gluon matter, Nucl.Phys. A498 (1989) 151c u.

  24. Yuri Sinyukov „Length of homogeneity”

  25. CorrelationWorkshops

  26. Expectations for RHIC...

  27. ...and unexpectedresultsfrom RHIC...

  28. HBT Excitation Function

  29. “RHIC HBT puzzle” STAR 130 GeV PHENIX 130 GeV • unexpected (small) sizes • Rout/Rside = (approx.)1 • Pt dependence do not agree with models • The same Pt dependence for pp, dAu and AuAu

  30. STAR DATA (pp,dAu,CuCu,AuAu@62GeV - prelim.) RHIC/AGS/SPS Systematics <kT>≈ 400 MeV (RHIC)<kT>≈ 390 MeV (SPS) Lisa, Pratt, Soltz, Wiedemann, nucl-ex/0505014 Pion HBT radii from different systems and at different energies scale with (dNch/dη)1/3

  31. System expansion: Initial vs Final Size Collisions at 200GeV only Smooth expansion of the system from p+p to Au+Au AuAu: system expands pp (dAu): no or less expansion • Proton initial size = 0.89 fm from e-scattering

  32. 0.2 0.3 0.4 0.5 0.2 0.3 0.4 0.5 0.6 Transverse mass dependence in Au+Au STAR, Au+Au@200GeV, PRC71 (2005) 044906 0. 0. 0. .2 Calc. with Blast-Wave -Retiere, Lisa,PRC 70 (2004) 044907 In Au+Au pT (mT) dependence attributed to collective expansion of the source

  33. Consistency check on flow – kaons

  34. Hania Gos, Kromeriz’05

  35. More confirmation STAR preliminary

  36. Surprising („puzzling”) scaling Ratio of (AuAu, CuCu, dAu) HBT radii by pp • All pT(mT) dependences of HBT radii observed bySTAR scale with pp although it’s expected that different origins drivethese dependences HBT radii scale with pp Scary coincidence or something deeper? pp, dAu, CuCu - STAR preliminary

  37. Catching up • Effective interaction time larger • Stronger correlation C- Moving away • Effective Interaction time smaller • Weaker correlation C+ “Double” ratio • Sensitive to the space-time asymmetry in the emission process C+ C- 1 R.Lednicky, V. L.Lyuboshitz, B.Erazmus, D.Nouais, Phys.Lett. B373 (1996) 30. k* Adam Kisiel, Fabrice Retiere Nonidentical particle correlations – the asymmetry analysis Heavier particle faster Lighter particle faster Kinematics selection along some direction e.g. kOut, kSide, cos(v,k)

  38. Pion-Kaon at 200 AGeV kaon faster pion faster STAR preliminary • Good agreement for same-charge combinations • Clear emission asymmetry signal Out double ratio Side double ratio + 0.9 syst. Sigma: 17.3± 0.8fm - 1.6 syst. + 6.1 syst. Mean: -7.0±1.2 fm - 4.0 syst.

  39. Pion-Proton 130 AGeV proton faster pion faster • Good agreement for identical and opposite charge combinations • We observe Lambda peaks at k*~decay momentum of Λ Λ peaks STAR preliminary Side double ratio Sigma: 15.1± 0.4 fm + 1.0 syst. - 1.5 syst. Mean: -7.4± 0.9 fm + 1.9 syst. - 3.4 syst. Out double ratio Fit assumes source is a gaussian in r*out

  40. Hania Gos, Kromeriz’05

  41. Adam Kisiel, Kromeriz’05 Origins of asymmetry pion emission times • Measures asymmetry in pair rest frame is a combination of time and space shifts in source frame • In heavy-ion collisions one expects difference in emission time from resonance decays all primordial pion average = 16.1 kaon average = 14.8 time shift = 1.3 kaon emission times all THERMINATOR calculation primordial

  42. pion emission points Space asymmetry from flow side • Transverse momentum of particles is composed of the thermal (randomly distributed) and flow (directed “outwards”) components • With no flow average emission point is at center of the source and the length of homogeneity is the whole source • Flow makes the source smaller (“size”-p correlation) AND shifted in outwards direction (x-p correlation) • For particles with large mass thermal motion matters less – they are shifted more in “out” direction. The difference is measured as emission asymmetry. out kaon emission points proton emission points THERMINATOR calculation

  43. Ry Rx Time Fourier coefficients of HBT() oscillations initial = final • Out-of-plane sources at freeze-out • Pressure and/or expansion time was not sufficient to quench initial shape • From v2 we know... • Strong in-plane flow → significant pressure build-up in system eccentricity  Short expansion time plays dominant role in out-of-plane freeze-out source shapes STAR Collaboration, nucl-ex/0312009

  44. Dmitri PeresounkoDirect photon interferometry PHENIX; d+Au collisions at √sNN=200 GeV

  45. Future plans at LHC

  46. RHIC/AGS/SPS Systematics ...and expectations for LHC <kT>≈ 400 MeV (RHIC)<kT>≈ 390 MeV (SPS) Assuming the same tendency: 40961/3=16 80001/3=20 Rexpected < 10fm

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