European Science Foundation Exploratory Workshop How to Constrain the High Density Symmetry Energy

1. 1950 – 2010 European Science Foundation Exploratory Workshop How to Constrain the High Density Symmetry Energy HiDeSymEne Z. Basrak, convenor Zoran Basrak Laboratory for Nuclear Physics Division of Experimental Physics RuđerBošković Institute, Zagreb, Croatia Strategic Workshop European Science Foundation Standing Committee for Physical and Engineering Sciences September 1, 2010, Egelsbach, Germany

2. ESF EW HiDeSymEne https://www.irb.hr/users/mkis/

3. Nucleosynthesis

4. p pV = nRT T SOFT V HARD E(,I) =E (,0) + Esym()I2 + o (I4) + ... I = (n− p) / Esym() ≈E()neutr. matter - E()sym. nucl. matter Nuclear Equation of state (EoS)

5. Symmetry energy • The density dependence of symmetry energy is largely unconstrained. • What is “stiff” or “soft” (curvature) is density dependent Z. Xiao et al., PRL102 (2009) 062502 The asymmetry term contributes a greater uncertainty than does the symmetric matter EOS. (Bao-An Li)

6. J. M. Lattimer and M. Prakash, Phys. Rep. 442 (2007) 109 Neutron star p / n≤ 0.1 – 0.2 c≤ (2-15)0 J. M. Lattimer and M. Prakash, Nucl. Phys. A777 (2006) 479

7. Z.Q. Feng, G.M. Jin, PL B683 (2010) 140 (Courtesy of M.B. Tsang) Supra-saturation densities The only available data (FOPI and FOPI–LAND collaborations @ GSI) result in a contradictory predictions for Esym: • n-p squeeze-out data from Au+Au collisions at E = 400A MeV [Y. Leifels et al., PRL 71 (1993) 963] →the UrQMD code predicts a steady rise of Esym → γ=0.60.3[W. Trautmann et al., ProgPartNuPh (2009)]. • n-p squeeze-out data from Au+Au collisions at E = 400A MeV [Y. Leifels et al., PRL 71 (1993) 963] →the UrQMD code predicts a steady rise of Esym → γ=0.60.3[W. Trautmann et al., ProgPartNuPh (2009)]. • π-/π+ yield ratio data for Au+Au collisions in a broad energy range [Reisdorf et al., NP A781 (2007) 459] →the IBUU04 code predicts a vanishing Esym → γ=0.960.21, super soft asyEOS[Z. Xiao et al., PRL 102 (2009) 062502].

8. HiDeSymEne Follow-up activities

9. European Science Foundation Research Networking Programmes Constraining the Symmetry Energy CoSymE Z. Basrak, M. Colonna and W. Trautmann

10. GDR & PYGNY RESONANCE How ?

11. What for ? • Creation of discussion fora: - theoreticians – experimentalists - nuclear physics – astrophysics • Exchange of students & experts • Facilitate a global dimension (complementarities) • Timely initiative • Prepare future - new intensive RIB facilities - train up a new generation of scientists to take over leadership • Open character

12. Who ? European Science Foundation 30 member states

13. Who ?

14. CoSymE proposal assessment

15. Presentations at meetings

16. Lobbying for CoSymE

17. Lund-SdC Califa MSU miniball .5 m IPJ phoswich GSI LAND LNS Chimera SIS18 ASY-EOS experiment S394 Experiment approved by GSI-PAC ASY-EOS Collaboration Zagreb, Croatia Caen, Orsay, France Darmstadt, Frankfurt, Germany Ioannina, Greece Catania, Milano, Napoli, Italy Katowice, Krakow, Warsaw, Poland Bucharest, Romania Santiago de Compostela, Spain Lund, Malmo, Sweden Daresbury, Liverpool, United Kingdom Kolkata, India NSCL-MSU, Rochester, USA

18. 1950 – 2010 European Science Foundation Exploratory Workshop How to Constrain the High Density Symmetry Energy HiDeSymEne Z. Basrak, convenor Thank you for your attention Zoran Basrak Laboratory for Nuclear Physics Division of Experimental Physics RuđerBošković Institute, Zagreb, Croatia Strategic Workshop European Science Foundation Standing Committee for Physical and Engineering Sciences September 1, 2010, Egelsbach, Germany