Kenji Morita 新学術領域研究「実験と観測て解き明かす中性子星の核物質」 L‐L Interaction from Relativistic Heavy Ion Collisions Kenji Morita (YITP, Kyoto) in Collaboration with Akira Ohnishi (YITP) Takenori Furumoto (Ichinoseki National Col.) Ref.) arXiv: 1408.6682 2014 Sep. 23 1 Kenji Morita (YITP, Kyoto) Role of LL Interaction Possible Emergence of Hyperons in NS core To understand EoS, Information on Hyperon‐Hyperon Interaction is indispensable Possible Existence of H‐dibaryon from KEK.jp 2014 Sep. 23 新学術領域研究「実験と観測て解き明かす中性子星の核物質」 2/15 Kenji Morita (YITP, Kyoto) RHIC Can Tell Us about LL interaction Au+Au 200AGeV ×108 events (60‐80%) (0‐5%) p p p p N N p1 L N p p N p N L p p Statistical Hadronization ~5 fm/c, ~160MeV 2014 Sep. 23 N p2 p time 新学術領域研究「実験と観測て解き明かす中性子星の核物質」 3/15 Kenji Morita (YITP, Kyoto) LL Correlation in HIC L Independent (Chaotic) emission (←Thermal Source) Identical particle correlation from quantum statistics (HBT effect) R C(Q) : effective source size L LL Interaction 1 Affects C(Q) when effective range reff is comparable with R Different results for repulsive and attractive interaction 0.5 C(Q) 2014 Sep. 23 新学術領域研究「実験と観測て解き明かす中性子星の核物質」 4/15 Kenji Morita (YITP, Kyoto) Analysis by STAR Coll. arXiv:1408.4360 Fit w/ Lednicky‐Lyuboshitz model Data: long tail (→ Small source size) Introduce “residual correlation” for a better fit to data HBT (size r0) 1.006 2014 Sep. 23 0.18 2.96 fm Interaction Residual correlation ‐0.044 新学術領域研究「実験と観測て解き明かす中性子星の核物質」 0.43 fm 5/15 Kenji Morita (YITP, Kyoto) Our Approach : Thermal Source + VLL Formula (Gong et al., ‘91) Emission source func. Thermal source model (Mimic hydro) Static Spherically Symmetric Spherically Symmetric + Hubble Flow Cylindrically Symmetric + Boost‐ invariance + Transverse flow 2014 Sep. 23 LL relative wave func. Various potentials Nijmegen model D, F, Soft Core89/97, ESC08 Ehime Quark model (fss2) Filikhin‐Gal (FG) Hiyama et al. (HKMYY) 新学術領域研究「実験と観測て解き明かす中性子星の核物質」 6/15 Kenji Morita (YITP, Kyoto) Potential, Wave func., / Correlation Correlation Function for the Static Source HBT (size R) Interaction : deviation from free w.f. Input VLL 2014 Sep. 23 新学術領域研究「実験と観測て解き明かす中性子星の核物質」 7/15 Kenji Morita (YITP, Kyoto) Results from the Static Source Strong attraction is reflected onto C(Q) Larger variation among potentials than data error‐bars Size : determined from min. c2 2014 Sep. 23 新学術領域研究「実験と観測て解き明かす中性子星の核物質」 8/15 Kenji Morita (YITP, Kyoto) Collectivity Deforms Source Function Influence on the best‐fit potentials? 2014 Sep. 23 C(Q) is fairly sensitive to interaction 新学術領域研究「実験と観測て解き明かす中性子星の核物質」 9/15 Kenji Morita (YITP, Kyoto) Collectivity Deforms Source Function Expanding Source Expansion velocity Boltzman factor with collective flow 50MeV 500MeV KM et al., PRC’00 2014 Sep. 23 新学術領域研究「実験と観測て解き明かす中性子星の核物質」 10/15 Kenji Morita (YITP, Kyoto) Illustration : Spherical Source Expansion makes the apparent source size smaller Attraction in C(Q) becomes stronger 2014 Sep. 23 新学術領域研究「実験と観測て解き明かす中性子星の核物質」 11/15 Kenji Morita (YITP, Kyoto) Illustration : Boost invariant Source Give a finite longitudinal extent Width of C(Q) (Q=|p1‐p2|) : effective 3d size Large RL : narrow width Transverse flow: fit to pt distribution of L (STAR ’12) 2014 Sep. 23 新学術領域研究「実験と観測て解き明かす中性子星の核物質」 12/15 Kenji Morita (YITP, Kyoto) Results from Boost‐invariant Source Effect of hf is rather small : longitudinal expansion dominates C(Q) Behavior at small Q is different from the static source ! 2014 Sep. 23 新学術領域研究「実験と観測て解き明かす中性子星の核物質」 13/15 Kenji Morita (YITP, Kyoto) Combined effects from flow and VLL (min. c2 against R) Effect of hf is absorbed into change of Ropt Longitudinal expansion gives another type of “best fit” 2014 Sep. 23 新学術領域研究「実験と観測て解き明かす中性子星の核物質」 14/15 Kenji Morita (YITP, Kyoto) VLL from RHIC Same VLL are chosen with smaller R! 2014 Sep. 23 新学術領域研究「実験と観測て解き明かす中性子星の核物質」 15/15 Kenji Morita (YITP, Kyoto) Summary & Discussion ‐1.8 < 1/a0 < ‐0.8 [fm‐1] 3.5 < reff < 7 [fm] Origin of long tail in STAR data? / Small source size? Long‐lived resonance (S0) Discrepancy from Nagara event? 2014 Sep. 23 新学術領域研究「実験と観測て解き明かす中性子星の核物質」 16/15
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