Concluding Remarks. W. Trautmann, GSI Helmholtzzentrum Darmstadt, Germany
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1 Concluding Remarks W. Trautmann, GSI Helmholtzzentrum Darmstadt, Germany
2 Olivier Lopez Angelo Pagano Sherry Yennello Zhigang Xiao Dominique Durand Patrick St.-Onge Jack Winkelbauer Alan McIntosh Giuseppe Politi Simone Valdré
3 n/p effective mass splitting Bill Lynch Pierre Morfouace Kyle Brown
4 SπRIT Experiment Betty Tsang Kaneko Masanori Nishimura Mizuki SπRIT TPC and ancillary detectors are installed inside the SAMURAI magnet so as to obtain as much as uniform magnetic field inside the field cage. Jerzy Łukasik Tadaaki Isobe NeuLAND is placed at 8.8 m from the target at the angle of 30 degrees., Slide 4
5 model dependence figure from Wenmei Guo et al., PLB 738, 197 (2014) elliptic flow ratio (FOPI-LAND) pion ratios (from analyses of the same FOPI exp. data) 5
6 Che-Ming Ko Dan Cozma Christoph Hartnack Natsumi Ikeno
7 Comparison of heavy-ion transport simulations: Collision integral in a box Yingxun Zhang ( 张英逊 ) China Institute if Atomic Energy Yongjia Wang, Maria Colonna, Pawel Danielewicz, Akira Ono, Betty Tsang, Hermann Wolter, Jun Xu, Lie-Wen Chen, Dan Cozma, Zhao-Qing Feng, Che-Ming Ko, Bao-An Li, Qing- Feng Li, S. Das Gupta, N. Ikeno, C.M. Ko, B.A.Li, Q.F.Li, Z.X. Li, S. Mallik, T. Ogawa, D. Oliinychenko, M. Papa, H. Petersen, Jun Su, Taesoo Song, Janus Weil, Ning Wang, Feng-Shou Zhang, Guo-Qiang Zhang, and Zhen Zhang,..
8 Akira Ono
9 peripheral 600 AMeV central Xe + 50 AMeV Arnaud Le Fèvre Akira Ono
10 fluctuations and correlations Paolo Napolitani Maria Colonna Hermann Wolter Yoritaka Iwata Hua Zheng
11 short range correlations? Subedi et al., 2008
12 EOS: RMF with density dependent couplings Stefan Typel
13 RIKEN 2010 astrophysics
14 Sandrine Courtin Carbon burning: a crucial phase in the stellar nucleosynthesis M < 8-9 M -> these stars are expected to shed their envelopes during helium burning and become white dwarfs, which may generate Type Ia supernovae M = 9-11 M -> burning could occur under a degenerate condition, carbon flash M > 11 M -> burning in a non-degenerate contracting core (T > 10 8 K, r > g.cm -3 ) Collision Accretion
15 25 Mio models from empirical parameters Francesca Gulminelli ChEFT + minimum constraint from neutron stars 11.5 < R < 13.5 km Hebeler, Lattimer, Pethick, Schwenk, ApJ 773 (2013) 11
16 neutron stars crust-core transition density and pressure Xavier Viňas Lie-Wen Chen Claudio Dorso Wei-Zhou Jiang Tsuyoshi Miyatsu Kazuhiro Oyamatsu Youngman Kim Shugaijam Singh to determine the mass-radius relationship in a neutron star requires the knowledge of the EOS in the core but also in the crust.
17 pasta phases in the transition region Sebastian Kubis
18 Hyperfragments production in the antiproton induced reactions Phys. Rev. C 93, (R) (2016) Zhao-Qing Feng NuSYM
19 hyperons in neutron stars J-Park) KISO event source: Kazuma Nakazawa, NSMAT2016,
20 the world average: L = MeV (L=3p 0 /ρ 0 ) Li and Han, PLB 727 (2013) ASY-EOS from n-skins neutron skins masses collective excitations isospin diffusion Maria Colonna Nils Paar observation of neutron stars crust oscillations r-mode instabilities mass-radius analysis 20
21 Kent Paschke Concettina Sfienti
22 sensitivity to density Bill Lynch FP variational Brown, PRL 85 (2000) Brown, PRL 111 (2013) 13 Skyrme sets fitted to ground-state properties of doubly magic nuclei E sym determined at 0.1 fm -3 neutron skin determines slope at 0.1 fm -3
23 status at present (GSI/FAIR) FOPI Yvonne Leifels ASY-EOS model predictions from Fuchs and Wolter, EPJA 30 (2006) APR graphics by Y. Leifels 23
24 sensitivity to density Dan Cozma using Tübingen QMD Difference of Elliptic-Flow Ratio Yongjia Wang Paolo Rusotto Yvonne Leifels ρ switch P. Russotto et al., PRC 94, (2016) 24
25 ASY-EOS: symmetry pressure p 0 = 3.8 ± 0.7 MeV/fm 3 Bill Lynch neutron star pressure p 0 = 3.4 ± 0.7 MeV/fm 3 ρ 0 Steiner, Lattimer, and Brown, ApJ 765, L5 (2013) 25
26 ASY-EOS II proposal Paolo Rusotto GSI-PAC in 2 weeks
27 opportunities for astrophysical observations NICER on the ISS Neutron-star Interior Composition Explorer 56 X-ray concentrators ( kev, 100 ns) measures time resolved X-ray emissions of neutron stars launched on June 3, 2017, at 17:07 EDT NICER science program begins July 13 source:nasa
28 Type I X-ray burst with oscillations, June 25, 2017 source:nasa
29 gravitational light bending ±5% (3σ)
30 EOS: lattice predictions arxiv: v4
31 Byungsik Hong
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