Light Antimatter Production in High Energy Collisions with DCPC Model Gang Chen China University of Geosciences, Wuhan Collaborators Yu-Liang Yan, Ben-Hao Sa (CIAE, China) Dai-Mei zhou (CCNU, China) 中国物理学会高能物理分会第九届全国会员代表大会暨学术年会

Found hypernuclei Analysis Method The Results in pp collision and AuAu collision Summary Outline 中国物理学会高能物理分会第九届全国会员代表大会暨学术年会

Found hypernuclei 中国物理学会高能物理分会第九届全国会员代表大会暨学术年会

4 from Hypernuclei to Neutron Stars hypernuclei  -B Interaction Neutron Stars S=-1 S=-2 S=- 0 Propose Several possible configurations of Neutron Stars – Kaon condensate, hyperons, strange quark matter J.M. Lattimer and M. Prakash, "The Physics of Neutron Stars", Science 304, 536 (2004) J. Schaffner and I. Mishustin, Phys. Rev. C 53 (1996): Hyperon-rich matter in neutron stars Saito, HYP06 中国物理学会高能物理分会第九届全国会员代表大会暨学术年会

5 Tracks in TPC It is first fonud nuclear contain anti-strange quark; The chart of nuclides is expand to the new anti-strange matter region.

6 70±17 antihypertritons 157 ±30 hypertritons About 89 million minimum-bias events 22 million most central collisions events STAR, Science 328 (2010) 58 Measured invariant hypernuclei yields 中国物理学会高能物理分会第九届全国会员代表大会暨学术年会

Measured invariant ratios 中国物理学会高能物理分会第九届全国会员代表大会暨学术年会

N. Sharma ( ALICE) J.Phys.G 38 (2011);arXiv: v2 Raw yield of anti deuterons as a function transverse momentum Production of antinuclei in pp collisions at 7 TeV with ALICE at the LHC Found hypernuclei in the high energy collision exp. 中国物理学会高能物理分会第九届全国会员代表大会暨学术年会

Observation of the antimatter helium-4 nucleus with the STAR Collaboration Found hypernuclei in the high energy collision exp. (STAR) N AT U R E ( ) 中国物理学会高能物理分会第九届全国会员代表大会暨学术年会

So we try to proposed a dynamically constrained phase space coalescence model + PACIAE model and used to investigate the production of light nuclei (anti-nuclei) in high energy collisions. The discovery for hypernuclei in the high energy experiment have been widely fascinating the sights of nuclear physicists. 中国物理学会高能物理分会第九届全国会员代表大会暨学术年会

Analysis Method PACIAE model 1. The string fragmentation in PYTHIA is switched-off temporarily and the diquarks (anti-diquarks) are broken randomly into quarks (antiquarks), so the parton initial state is obtained. 2. The parton rescattering is proceeded until partonic freez-out. 3. Then the hadronization is followed. 4. At last the hadronic rescattering is proceeded until hadronic freez-out. Ben-Hao Sa,etal. Comput. Phys. Commun., 183, 333 (2012). It is the parton and hadron cascade Model based on PYTHIA. 中国物理学会高能物理分会第九届全国会员代表大会暨学术年会

Analysis Method Dynamically constrained phase space coalescence model In the theoretical studies, the yield of light nuclei (anti-nuclei) is usually calculated in two steps: (1)The nucleons and hyperons are calculated by the transport model. (2)The light nuclei (anti-nuclei) are calculated by the phase space coalescence model with Wigner function or by the statistical model. This coalescence model strongly relies upon the assumption of light nuclei (anti-nuclei) wave function used to construct the Wigner function. The statistical model strongly relies upon the equilibrium assumption and the fitted temperature and baryon chemical potential. We proposed a dynamically constrained phase space coalescence model to calculate the yield of light nuclei (anti-nuclei) after the transport model simulations. Ben-Hao Sa,etal. Comput. Phys. Commun., 183, 333 (2012). Yu-Liang Yan, Gang Chen et al, Phys. Rev. C (2012). 中国物理学会高能物理分会第九届全国会员代表大会暨学术年会

As the uncertainty principle one can only say particle lies somewhere within a six dimension quantum ``box" or “state" of volume of ΔqΔp However,we can estimate the yield of a single particle by Similarly for the yield of N particles cluster Dynamically constrained phase space coalescence model 中国物理学会高能物理分会第九届全国会员代表大会暨学术年会

The yield of, for instance, is assumed to be Dynamically constrained phase space coalescence model m 0 and D 0 stand for the rest mass and diameter of Δm refers to the allowed uncertainty. 中国物理学会高能物理分会第九届全国会员代表大会暨学术年会

The Results in p+p coll. The model parameters are fitted to the STAR data of strange particles as shown in the following table. TABLE I: Particle yield in NSD pp collisions at = 0.2 TeV. B. I. Abelev, et al., STAR, Phys. Rev. C (2007). Then they are used to calculate the yield of D, 3 He, and, etc., Yu-Liang Yan, Gang Chen et al, Phys. Rev. C (2012). 中国物理学会高能物理分会第九届全国会员代表大会暨学术年会

The Results of Hadron and light (anti)nuclei in p+p coll. Hadron and light nuclei (anti- nuclei) yields in NSD p+p collisions at =7 and 14 TeV calculated by final hadronic state in the PACIAE and PYTHIA simulations. a Calculated with △ m= GeV. b Estimated from ALICE Data, J.Phys.G 38(2011) c Calculated with △ m=0.005 GeV. predict the light (anti)nuclei yield in pp collisions at √s = 7 and 14 TeV. 中国物理学会高能物理分会第九届全国会员代表大会暨学术年会

The Results in p+p coll. FIG. 1: Transverse momentum distributions of light anti-nuclei in the NSD pp collisions at = 7 and 14 TeV with PACIAE and PYTHIA model The green dots are ALICE data. 中国物理学会高能物理分会第九届全国会员代表大会暨学术年会

FIG. 1: Rapidity distributions of light anti-nuclei in the NSD pp collisions at =7 and 14 TeV with PACIAE and PYTHIA model The Results in p+p coll. The strong fluctuation, indicates that the 1.2 x10 8 events are not enough for the p T and y distribution of the particles. 中国物理学会高能物理分会第九届全国会员代表大会暨学术年会

The Results in Au+Au coll. at =200 GeV Chen Gang Yu-Liang Yan et al, PRC 86, (2012) The model parameters are fitted to the STAR data of strange particles as shown in the following table. Then they are used to calculate the yield of D, 3 He, and, etc., STAR a, PRL 98, (2007) A. Andronic et al., PLB 697, 203 (2011) Hadron yields from Model in comparison with the STAR data Obviously, the model results are very close to the data exp 中国物理学会高能物理分会第九届全国会员代表大会暨学术年会

f Δm= GeV. b Δm= GeV. Light (anti)nuclei yields of models in comparison with the STAR The yields in PACIAE model simulation are consistent with STAR data. egh The STAR, Science 328, 58 (2010); a L. Xue,Y. G. Ma et al.,PRC (2012). c A. Andronic,et al., PLB 697(2011) The Results in Au+Au coll. at =200 GeV Chen Gang et al, PRC 86, (2012) 中国物理学会高能物理分会第九届全国会员代表大会暨学术年会

The comparison of particles ratios between data and model calculations. The Results in Au+Au coll. at = 200 GeV Δm= GeV for D, Δm= GeV for,,, Δm= GeV for D, Δm= GeV for,,, The STAR yield ratios are good reproduced. Light (anti)nuclei ratio in comparison with the STAR data Chen Gang et al, PRC 86, (2012) 中国物理学会高能物理分会第九届全国会员代表大会暨学术年会

Transverse momentum distributions of light (anti)nuclei. The Results in Au+Au coll. at =200 GeV Chen Gang et al, PRC 86, (2012) 中国物理学会高能物理分会第九届全国会员代表大会暨学术年会

The Centrality dependence of light anti-nuclear produced in Au+Au coll. Chen Gang et al, PRC 88, (2013) FIG. 1. The integrated yield dN/dy of strange particle at midrapidity Au+Au collisions at 200 GeV as a function of centrality. 中国物理学会高能物理分会第九届全国会员代表大会暨学术年会

Chen Gang et al, PRC 88, (2013) The Centrality dependence of light anti-nuclear produced in Au+Au coll. TAB I: Integrated yields dN/dy calculated by PACIAE+DCPC model. Δm= GeV for D, ; Δm= GeV for,,, 中国物理学会高能物理分会第九届全国会员代表大会暨学术年会

The Centrality dependence of light anti- nuclear produced in Au+Au coll. FIG. 2: Light nuclei and anti-nuclei cumulative yields STAR,Science 328, 58 (2010) STAR,arXiv: PHENIX, PRL. 94, (2005). The yields in PACIAE model simulation are consistent with Exp. data. Chen Gang et al, PRC 88, (2013) 中国物理学会高能物理分会第九届全国会员代表大会暨学术年会

The Centrality dependence of light anti-nuclear produced in Au+Au coll. Chen Gang et al, PRC 88, (2013) FIG. 3: The normalized yield y c Defined a normalized yield The curves are fitted by Theoretical and exp. results of yields in different centrality bins can be converted into the constant yield Y MB for direct comparison. 中国物理学会高能物理分会第九届全国会员代表大会暨学术年会

The Centrality dependence of light anti- nuclear produced in Au+Au coll. Chen Gang et al, PRC 88, (2013) FIG. 4: Yield ratios The yield ratios of also remain unchanged from central to peripheral coll. 中国物理学会高能物理分会第九届全国会员代表大会暨学术年会

Scaling Properties of light antinuclei production in Au+Au coll. L. Xue,Y. G. Ma,PRC85, (2012) STAR, Nature 473,353 (2011); Hecke, Sorge, Xu, PRL. 81, 5764 (1998). Figure 1:

Scaling Properties of light antinuclei production in Au+Au coll. 中国物理学会高能物理分会第九届全国会员代表大会暨学术年会 Figure 2: Atomic number dependence of the integrated yield dN/dy of light (anti)nuclei in different centrality bins. 149MeV for 0-5%, 142 MeV for MB, 125 MeV for 40-60% Chen Gang, arXiv: , 2014

Scaling Properties of light antinuclei production in Au+Au coll. The existence of a mass scale properties? 中国物理学会高能物理分会第九届全国会员代表大会暨学术年会 Chen Gang, arXiv: , 2014

Scaling Properties of light antinuclei production in Au+Au coll. Defined a ratio of yield per N part 中国物理学会高能物理分会第九届全国会员代表大会暨学术年会 Figure 3: The integrated yield dN/dy at midrapidity divided by Npart, normalized to the peripheral collisions (40-60%),.

Summary 中国物理学会高能物理分会第九届全国会员代表大会暨学术年会 We proposed a dynamically constrained phase space coalescence model to calculate the light (anti)nuclei in high enerngy collisions, The results turned out that it would be an effective method investigating the production of light (anti)nuclei in high energy collisions. Predict the light (anti)nuclei yield, transverse momentum and the rapidity distribution in pp collisions at √s = 7 and 14 TeV. Study centrality dependence of light anti-nuclear produced in Au+Au collisions. Discussed the scaling properties of light antinuclei production in Au+Au collisions.

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35 Larry,Robert. Pisarski,NPA 796, 83, Torrieri, Vogel, Bauchle,PRL111, , 2013.