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Investigation of effective interactions in relativistic mean field theory
KTH, School of Engineering Sciences (SCI), Physics.
2005 (English)Licentiate thesis, comprehensive summary (Other scientific)
Place, publisher, year, edition, pages
Stockholm: KTH , 2005. , 83 p.
Series
Trita-FYS, ISSN 0280-316X ; 2005:29
National Category
Subatomic Physics
Identifiers
URN: urn:nbn:se:kth:diva-4074ISBN: 91-7178-093-9 (print)OAI: oai:DiVA.org:kth-4074DiVA: diva2:10641
Presentation
2005-07-07, , AlbaNova, Stockholm, 10:00
Note
QC 20101123Available from: 2006-08-17 Created: 2006-08-17 Last updated: 2010-11-23Bibliographically approved
List of papers
1. Density dependencies of interaction strengths and their influences on nuclear matter and neutron stars in relativistic mean field theory
Open this publication in new window or tab >>Density dependencies of interaction strengths and their influences on nuclear matter and neutron stars in relativistic mean field theory
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2004 (English)In: Physical Review C. Nuclear Physics, ISSN 0556-2813, E-ISSN 1089-490X, Vol. 69, no 4Article in journal (Refereed) Published
Abstract [en]

The density dependencies of various effective interaction strengths in the relativistic mean field are studied and carefully compared for nuclear matter and neutron stars. The influences of different density dependencies are presented and discussed on mean field potentials, saturation properties for nuclear matter, equations of state, maximum masses, and corresponding radii for neutron stars. Though the interaction strengths and the potentials given by various interactions are quite different in nuclear matter, the differences of saturation properties are subtle, except for NL2 and TM2, which are mainly used for light nuclei, while the properties by various interactions for pure neutron matter are quite different. To get an equation of state for neutron matter without any ambiguity, it is necessary to constrain the effective interactions either by microscopic many-body calculations for the neutron matter data or the data of nuclei with extreme isospin. For neutron stars, the interaction with large interaction strengths give strong potentials and large Oppenheimer-Volkoff (OV) mass limits. The density-dependent interactions DD-ME1 and TW-99 favor a large neutron population due to their weak rho-meson field at high densities. The OV mass limits calculated from different equations of state are 2.02-2.81M, and the corresponding radii are 10.78-13.27 km. After the inclusion of the hyperons, the corresponding values become 1.52-2.06M and 10.24-11.38 km.

Keyword
hartree-bogoliubov description, halo, energy
National Category
Subatomic Physics
Identifiers
urn:nbn:se:kth:diva-6051 (URN)10.1103/PhysRevC.69.045805 (DOI)000221427500061 ()
Note
QC 20100623Available from: 2006-08-17 Created: 2006-08-17 Last updated: 2017-12-14Bibliographically approved
2. Nuclear symmetry energy in relativistic mean field theory
Open this publication in new window or tab >>Nuclear symmetry energy in relativistic mean field theory
2006 (English)In: Physics Letters B, ISSN 0370-2693, E-ISSN 1873-2445, Vol. 633, no 2-3, 231-236 p.Article in journal (Refereed) Published
Abstract [en]

The physical origin of the nuclear symmetry energy is studied within the relativistic mean field (RMF) theory. Based on the nuclear binding energies calculated with and without mean isovector potential for several isobaric chains we confirm earlier Skyrme-Hartree-Fock result that the nuclear symmetry energy strength depends on the mean level spacing epsilon(A) and an effective mean isovector potential strength K(A). A detailed analysis of the isospin dependence of these two components contributing to the nuclear symmetry energy reveals a quadratic dependence due to the mean-isoscalar potential, similar to epsilon T-2, and, completely unexpectedly, the presence of a strong linear component similar to kappa T(T + 1 + epsilon/kappa) in the isovector potential. The latter generates a nuclear symmetry energy in RMF theory that is proportional to E-sym similar to T(T + 1) at variance to the non-relativistic calculation. The origin of the linear term in RMF theory needs to be further explored.

Keyword
relativistic mean field; nuclear symmetry energy; mean level density; isovector potential
National Category
Subatomic Physics
Identifiers
urn:nbn:se:kth:diva-7391 (URN)10.1016/j.physletb.2005.11.077 (DOI)000235098500016 ()2-s2.0-30944467234 (Scopus ID)
Note
QC 20100623Available from: 2007-08-20 Created: 2007-08-20 Last updated: 2017-12-14Bibliographically approved

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