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Constraints on EOS from finite nuclei, heavy ion collisions and neutron stars

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Constraints on EOS from finite nuclei, heavy ion collisions and neutron stars (EN)
Wolter, H. H.
Gaitanos, T.
Di Toro, M.
Colonna, M.
Ferini, G.
Lalazissis, G. A.
info:eu-repo/semantics/article
info:eu-repo/semantics/publishedVersion
2020-01-01
We present several possibilities offered by nuclear structure, the dynamics of intermediate energy heavy ion collisions and neutron stars to investigate the nuclear matter equation of state (EoS) beyond the ground state. In particular the high density nuclear EoS of asymmetric matter, i.e. the symmetry energy, is discussed. (EN)
heavy ion collisions (EN)
equation of state (EN)
neutron stars (EN)
symmetry energy (EN)
strangeness ratio (EN)
maximum mass constraint (EN)
proton fraction (EN)
Nuclear matter (EN)
finite nuclei (EN)
Direct Urca process (EN)
Annual Symposium of the Hellenic Nuclear Physics Society
English
Hellenic Nuclear Physics Society (HNPS) (EN)
2654-0088
2654-007X
Annual Symposium of the Hellenic Nuclear Physics Society; Τόμ. 15 (2006): HNPS2006; 196-201 (EL)
HNPS Advances in Nuclear Physics; Vol. 15 (2006): HNPS2006; 196-201 (EN)
Πνευματική ιδιοκτησία (c) 2019 T. Gaitanos, G. Ferini, M. Colonna, M. Di Toro, G. A. Lalazissis, H. H. Wolter (EL)
Hellenic Nuclear Physics Society
Annual Symposium of the Hellenic Nuclear Physics Society
Oral contributions



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