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Workshop on Nuclear Structure and Astrophysical Application ,

Workshop on Nuclear Structure and Astrophysical Applications. „EOS day“ (Thursday, July 11) Convenors: F. Gulminelli (Caen), Y. Leifels (GSI).  chairpersons: H. Wolter (LMU Munich), H. Leeb (TU Wien). Workshop on Nuclear Structure and Astrophysical Application ,

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Workshop on Nuclear Structure and Astrophysical Application ,

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  1. Workshop on Nuclear Structure and Astrophysical Applications „EOS day“ (Thursday, July 11) Convenors: F. Gulminelli (Caen), Y. Leifels (GSI)  chairpersons: H. Wolter (LMU Munich), H. Leeb (TU Wien) Workshop on Nuclear Structure and Astrophysical Application, 3nd Thexo meeting, ECT*, Trento, July 8-12, 2013

  2. neutron matter EOS Symmetry energy: Diff. neutron and symm matter EOS of symmetric nuclear matter asy-stiff stiff asy-soft soft Investigate dependence in large part of (r,d)-plane rB/r0 Fairly well fixed! Soft Equation-of-State and Symmetry Energy BW mass formula symmetry energy density-asymmetry dep. of nucl.matt. density r asymmetry d Rather uncertain! esp. at high density Isovector tensor correlations?

  3. Constraints on EoS via Astrophysical Observation and Laboratory Experiments Model for structure of NS Heavy ion collisions

  4. Constraints on EoS via Astrophysical Observation and Laboratory Experiments Hadronic EoS‘s Strange and Quark EoS‘s Model for structure of NS Trümper Constraints (Universe Cluster, Irsee 2012) Observations of: masses radii (X-ray bursts) rotation periods etc

  5. Levels of description of evolution from initial to final state: initial final thermal Thermal expansion hydrodynamics transport theory Heavy ion collisons non-equilibrium

  6. T T T T QPA BUU transport equation Can be derived:  Classically from the Liouville theorem collision term added  Semiclassically from THDF (and fluctuations)  From non-equilibrium theory (Kadanoff-Baym) collision term included mean field and in-medium cross sections consistent, e.g. from BHF Spectral fcts, off-shell transport, quasi-particle approx. Transport theory is on a well defined footing, in principle

  7. time distribution of collisions (energy integrated) Code Comparison Project: Workshop on Simulations of Heavy Ion Collisions at Low and Intermediate Energies, ECT*, Trento, May 11-15, 2009  using same reaction and physical input (not neccessarily very realistic, no symm energy))  include major transport codes  obtain estimate of „systematic errors“ transverse flow • agreement for flow and other one-body observables reasonable, but perhaps not really good enough to make detailed conclusions • symmetry effects are order of magnitude smaller: hope that differences are less sensitive (?) • origin of differences: collisions ?

  8. p+/p- ratio, Feng, et al. Au+Au, elliptic flow, FOPI Present constraints on the symmetry energy from heavy ion collisions Esym(r) [MeV] Fermi energy HIC, various observables r/r0 p+/p- ratio B.A. Li, et al. Moving towards a determination of the symmetry energy in HIC but at higher density few data and some difficulty with consistent results of simulations for pion observables.

  9. Neutron star Mass-Radius relation Neutron star Constraints; allowed region heavy ion collisions in the Fermi energy regime Isospin Transport properties, (Multi-)Fragmentation p, n Hadronic EoS‘s Asy-stiff M. Colonna, A. Chbihi Esym(rB)(MeV) S. Typel, M. Oertel, N. Chamel G. Baym (ECT* Colloquium) rel. heavy ion collisions Asy-soft Nuclear structure (neutron skin thickness, Pygmy DR, IAS) Slope of Symm Energy 0 1 rB/r0 2 3 Isotopic ratios of flow, particle production D. Roissy, P. Russoto Investigations on the Nuclear Symmetry Energy An interesting day !

  10. Constraints on the slope of the symmetry energy from Structure and reactions A. Carbone, et al., PRC81, 043101 (2010) heavy ion collisions

  11. SE ist also momentum dependent  effective mass m*n < m*p Different proton/neutron effective masses m*n > m*p Isovector (Lane) potential: momentum dependence data The Nuclear Symmetry Energy in different „microscopic“ models Rel, Brueckner Nonrel. Brueckner Variational Rel. Mean field Chiral perturb. The EOS of symmetric and pure neutron matter in different many-body approaches C. Fuchs, H.H. Wolter, EPJA 30(2006)5 The symmetry energy (at T=0) as the difference between symmetric and neutron matter: SE r/r0 k [fm-1] Why is symmetry energy so uncertain in microscopic models?  In-medium r mass, and short range isovector tensor correlations (e.g. B.A. Li, PRC81 (2010))

  12. Constraints on EoS via Astrophysical Observation and Laboratory Experiments Model for structure of NS Quark-hadron phase transition Liquid-gas phase transition SIS 1 Supernovae IIa neutron stars 0 Z/N Isospin degree of freedom

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