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Masashi Kaneta, LBL Hadron Spectra in Au+Au Collisions by STAR Experiment at RHIC Masashi Kaneta for the STAR collaboration LBNL.

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Presentation on theme: "Masashi Kaneta, LBL Hadron Spectra in Au+Au Collisions by STAR Experiment at RHIC Masashi Kaneta for the STAR collaboration LBNL."— Presentation transcript:

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2 Masashi Kaneta, LBL Hadron Spectra in Au+Au Collisions by STAR Experiment at RHIC Masashi Kaneta for the STAR collaboration LBNL

3 Masashi Kaneta, LBLIntroduction Study of bulk properties Macroscopic approach –Chemical freeze-out –Thermal freeze-out Focusing on p T distribution –Thermal freeze-out Temperature –Transverse flow Time 核子核子 核子核子 核子核子 核子核子 核子核子 核子核子 核子核子 核子核子 核子核子 核子核子 核子核子 核子核子 核子核子 核子核子 核子核子 核子核子 核子核子 核子核子 核子核子 核子核子 核子核子 核子核子 核子核子 核子核子 核子核子 核子核子 Expansion Cooling

4 Masashi Kaneta, LBL RHIC-STAR experiment Solenoidal Tracker At RHIC ~40 Institutes/Universities ~300 Collaborators One of large experiments at RHIC 2  acceptance Excellent particle identification

5 Masashi Kaneta, LBL STAR Event Tracks are reconstructed by online tracking

6 Masashi Kaneta, LBL Particle Identification dE/dx by TPC : ,K,p,d,He,…… Kink method : K RICH : 1-3 GeV/c for /K, 1.5-5GeV/c for p Topology : K 0 s Combinatrics :   ……  K p e |p/Z| [GeV/c] dE/dx TOF (year 2) EMC (year 2)

7 Masashi Kaneta, LBL p T Distribution / Kinetic Freeze-out Kinetic freeze-out –End of elastic interactions –Information of momentum is frozen Boltzmann distribution + flow effect  No Boost Boosted Blast wave model; E. Schnedermann et al., PRC48(1993)2462

8 Masashi Kaneta, LBL p T distribution vs. Centrality p T [GeV/c] ]GeV/c)[( 2 2- 2 TT dp dyp nd   K  (dE/dx) p K  (dE/dx) K  (kink) K  (kink) p STAR Preliminary for K, p 345  7 280  9 235  8 180  9 135  8 100  4 70  4 25  3 for  345  7 289  9 221  4 152  9 102  4 63  4 35  3 20  2 9  4 ------- central peripheral

9 Masashi Kaneta, LBL Centrality dependence of T th and Centrality dependence of T th and As a function of centrality –T th ~ 100 MeV – goes up then saturated –Flow profile changed? Selected similar centrality region in and K,p  KK p KK p p T [GeV/c] ] GeV/c) [( 2 2- 2 T T dp dy p n d  38 115 224 347

10 Masashi Kaneta, LBL Bombarding Energy Dependence From SPS to RHIC –Increasing flow –Decreasing temperature –Longer time for cooling at RHIC? T th [GeV] [c] STAR PHENIX

11 Masashi Kaneta, LBLSummary The p T distributions of , K, and p are obtained as a function of centrality from RHIC-STAR at s NN =130GeV Au+Au The blast wave model describes the data over all of centrality As a function of centrality at RHIC –T th ~ 100 MeV – goes up then saturated (~0.55c) –Flow profile changed? From SPS to RHIC –Increasing flow –Decreasing temperature –Indicating longer time for cooling at RHIC?

12 Masashi Kaneta, LBL ] [GeV/ 2 2 c dy dp N d T  STAR PHENIX model STAR vs. PHENIX STAR vs. PHENIX PHENIX  and K show smaller yield at p T >0.6 than STAR –upto factor of 2!! Protons have coincidence  K+K+ K-K- p p

13 Masashi Kaneta, LBLCentrality centrality bin for kink K

14 Masashi Kaneta, LBL STAR Event

15 Masashi Kaneta, LBL Test of Flow Profile

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