1 / 17

Nuclear Isovector Equation-of-State (EOS) and Astrophysics

Nuclear Isovector Equation-of-State (EOS) and Astrophysics. Hermann Wolter Dep. f. Physik, LMU. Topics: Phase diagram of strongly interacting matter and exploration via heavy ion collisions Symmetric and asymmetric EoS, density dependence of symmetry energy

xantha-moody
Télécharger la présentation

Nuclear Isovector Equation-of-State (EOS) and Astrophysics

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. Nuclear Isovector Equation-of-State (EOS) and Astrophysics Hermann Wolter Dep. f. Physik, LMU • Topics: • Phase diagram of strongly interacting matter and exploration via heavy ion collisions • Symmetric and asymmetric EoS, density dependence of symmetry energy • Description of Heavy Ion collisions with transport equations • Some results from HI studies • Comparison to neutron star observables • Summary and Outlook

  2. Connection to Universe Cluster EoS, esp. Symmetry energy at high density Interpretation of heavy ion collision exp. (Astrophysical reaction rates by indirectmethods)

  3. Liquid-gas coexistence Quark-hadron coexistence Schematic Phase Diagram of Strongly Interacting Matter SIS

  4. Quark-hadron coexistence Schematic Phase Diagram of Strongly Interacting Matter SIS Liquid-gas coexistence 1 Exotic nuclei neutron stars 0 Z/N

  5. Vij Relativistic: Hadronic Lagrangian y, nucleon, resonances s,w, p,.... mesons Comparisons of calculations: Empirical saturation point Theoretical Treatment of Nuclear Matter Non-relativistic: Hamiltonian H = S Ti + S Vij,; V nucleon-nucleon interaction

  6. Symmetry energy iso-stiff stiff soft iso-soft The nuclear EoS-Uncertainties the nuclear EoS Esymm[MeV] C. Fuchs, H.H. Wolter, WCI book, EPJA 30 (2006 )5

  7. Transport Descriptions of Heavy Ion Collisions Heavy ion collisions -> Non-Equilibrium Phenomena -> Transport Theory

  8. 3 4 loss term gain term 1 2 Simulation with Test Particles: 1 1 1 Hamiltonian EoM test particles Transport description of heavy ion collisions: For Wigner transform of the one-body density: f(r,p;t) Vlasov eq.; mean field 2-body hard collisions

  9. Observables High Density Symmetric Nuclear Matter V1: Sideward flow V2: Elliptic flow T.Gaitanos, Chr. Fuchs, Nucl. Phys. 744 (2004)

  10. asysoft eos superasystiff eos experimental data (B. Tsang et al. PRL 92 (2004) ) Isospin Transport through Neck: Rami imbalance ratio: ASYSOFT EOS – FASTER EQUILIBRATION Baran, Colonna, Di Toro, Zielinska-Pfabe, Wolter, PRC 72 (2005) 064620

  11. Kaon Production: A good way to determine the symmetric EOS (C. Fuchs, A.Faessler, et al., PRL 86(01)1974) Main production mechanism: NNBYK, pNYK • Also useful for Isovector EoS? • charge dependent thresholds • in-medium effective masses • Mean field effects

  12. Equations of State tested: Astrophysical Implications of Iso-Vector EOS Neutron Star Structure Constraints on the Equation-of-state - from neutron stars: maximum mass gravitational mass vs. baryonic mass direct URCA process mass-radius relation - from heavy ion collisions: flow constraint kaon producton Klähn, Blaschke, Typel, Faessler, Fuchs, Gaitanos,Gregorian, Trümper, Weber, Wolter, Phys. Rev. C74 (2006) 035802

  13. Proton fraction and direct URCA Forbidden by Direct URCA constraint Onset of direct URCA Neutron star masses and cooling and iso-vector EOS Tolman-Oppenheimer-Volkov equation to determine mass of neutron star Heaviest observed neutron star Typical neutron stars

  14. Further Neutron Star Constraints: Mass-Radius Relation: Gravitational vs. Baryon Mass

  15. Gravitational vs. Baryon Mass Direct Urca Cooling limit Mass-Radius Relations Heavy Ion Collision obsevables Maximum mass

  16. Summary and Outlook: • Equation of State at high densities can be tested in the laboratory in heavy ion collisions • Symmetry Energy (neutron matter) is particularly uncertain • Is important for the structure of exotic nuclei (nucleosynthesis) and for astrophysics • Comparison to neutron star observables (not completely satisfactory, yet); also supernovae Collaborators: C. Fuchs (Tübingen), T. Gaitanos (Giessen) D. Blaschke, et al., (Rostock-Breslau) M. Di Toro, M. Colonna, et al., (LNS Catania)

More Related