Post on 20-Jan-2016
P. ArumugamCentro de Física das Interacções Fundamentais and Departamento de Física, Instituto Superior Técnico,
Lisbon, Portugal
S.K. Patra, P.K. Sahu, B.K. SharmaInstitute of Physics, Bhubaneswar, India
X. Vinãs, M. Centelles, Tapas SilUniversitat de Barcelona
Ladek Zdroj
28-Feb-2008
2Outline
Mean Field Theory
Quantum Hadrodynamics
EFT motivated Relativistic Mean Field (E-RMF) Theory
Finite Nuclei
Bulk properties justifying the fit & overall description
Halo & Clustering precision of evaluated density distributions
Neutron skin Neutron stars
Infinite Matter
EoS at high densities
Neutron star properties
Liquid-gas phase transition
Conclusions
3Quantum Hadrodynamics (QHD)
Earlier QHD studies were based on renormalizable models No scalar-vector & vector-vector interactions
“Standard” RMF models• Non-linear • Use effective coupling constans renormalizability ???
Modern approach to renormalization• Cutoff in derivative expansions• All non-renormalizable couplings consistent with the underlying
symmetries of QCD are allowed
4EFT motivated RMF: E-RMF
5The Energy Density Functional
6Some applications of E-RMF
Pion-nucleus scattering B. C. Clark et al, PLB 427, 231 (1998).
Nuclear spin-orbit force R. J. Furnstahl et al, NPA 632, 607 (1998).
Asymmetric nuclear matter at finite temperature (with G1) P. Wang, PRC 61, 054904 (2000).
Effect of new nonlinear couplings on the nuclear matter and finite nuclear properties
M. Del Estal et al, NPA 650, 443 (1999); PRC 63, 024314 (2001); PRC 63, 044321 (2001).
Superheavy nucleiT. Sil et al, PRC 69, 044315 (2004).
Reaction cross-sections in stable and unstable nucleiSharma et al, JPG 32, 2089 (2006); Shukla et al, PRC 76, 034601 (2007)
7Bulk properties of some nuclei
82n-separation energies
9Cluster & Halo structures
Arumugam et al, PRC 71, 064308 (2005)
Sharma et al, JPG 32, L1 (2006)
11Li
10Neutron skin in heavy nuclei
Uncertainty in neutron radius measurement ~ 0.2 fm !!
Only few popular Skyrme parameters relevant for finite nuclei are chosen.
Piekarewicz nucl-th/0607039v1 (2006),
Horowitz and Piekarewicz PRC 64, 062802R (2001)
11Dirac potentials at high density
12Energy at high densities
Coester band R. Brockmann and R. Machleidt, PRC 42, 1965 (1990).
13EoS is symmetric nuclear matter
Arumugam et al, PLB 601, 51 (2004).
14EoS in Neutron Matter
Arumugam et al, PLB 601, 51 (2004).
15Neutron Star Properties
Arumugam et al, PLB 601, 51 (2004).
16Phase transitions in nuclear matter
Arumugam et al, PLB 601, 51 (2004).
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18Recent work
Quark-Hadron phase transitions within E-RMF
Sharma, Panda and Patra, PRC 75, 035808 (2007).
Full octet of Baryons in the Lagrangian
No mixed phase with original G2 parameter set
G2* (G2): K = 300 (215), mN*/mN = 0.7 (0.664),
saturation properties were used to fix other constants
Unpaired quark matter & Color flavor locked quark matter
Many questions remain open
19Summary & Conclusions
E-RMF: Systematic inclusion of new interaction terms under the guidance of EFT techniques
No forcing of any change in the parameters initially determined from a few magic nuclei
Results for finite nuclei are as good as any best model or even better
Soft EOS both around saturation and at high densities which is consistent with
measurements of kaon production flow of matter in energetic heavy-ion collisions observed neutron star masses and radii
Liquid-gas phase transition is understood but questions remain open with Quark phase and G2*
E-RMF approach can be considered as a salient step towards a unified theory for finite nuclei as well as for infinite nuclear matter
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