Relativistic mean-field theory for unstable nuclei with non-linear σ and ω terms

Sugahara, Yuichi; Toki, H.

doi:10.1016/0375-9474(94)90923-7

Cited by 983 publications

(1,129 citation statements)

References 14 publications

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“…Here we find that sets IV and V match with NL3 and DBHF, respectively up to three times the nuclear matter density. It is to be noted that the EOS obtained by DBHF is trusted upto two times of nuclear matter density [36,37]. The difference between the two sets IV (stiff) and V (soft) is only due to the different effective mass for the same incompressibility (K = 300 MeV).…”

Section: At Zero Temperature Limitmentioning

confidence: 90%

Hot nuclear matter in asymmetry chiral sigma model

et al. 2004

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In the frame work of SU(2) chiral sigma model, the nuclear matter properties at zero and finite temperature have been investigated. We have analyzed the nuclear matter equation of state by varying different parameters, which agrees well with the one derived from the heavy-ion collision experiment at extreme densities and reliable realistic(DBHF) model at low density region. We have then calculated the temperature dependent asymmetric nuclear matter, also investigated the critical temperature of liquid gas phase transition and compared with the experimental data. We found that the critical temperature in our model is in the range of 14−20 MeV.

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Section: At Zero Temperature Limitmentioning

confidence: 90%

Hot nuclear matter in asymmetry chiral sigma model

et al. 2004

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“…For the treatment of nuclear interactions, we employ the relativistic mean-field (RMF) model with the TM1 parameter set [21], where nucleons interact via the exchange of isoscalar scalar and vector mesons (σ and ω) and isovector vector meson (ρ). The nucleonic Lagrangian density reads…”

Section: Relativistic Mean-field Model and Thomas-fermi Approximationmentioning

confidence: 99%

“…From the Lagrangian density (1), we derive the equations of motion for nucleons and meson mean fields, which can be solved self-consistently. The TM1 parametrization of the RMF model was found to be successful in describing the ground-state properties of finite nuclei and infinite nuclear matter [21]. In order to examine the influence of the symmetry energy slope L, we use a set of generated models based on the TM1 parametrization as described in our previous work [22].…”

Section: Relativistic Mean-field Model and Thomas-fermi Approximationmentioning

confidence: 99%

Finite-Size Effects on Equation of State for Supernovae and Neutron Stars

Shen

Bao

et al. 2018

Proceedings of the Workshop on Quarks and Compact Stars 2017 (QCS2017)

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We study the equations of state of nuclear matter and neutron-star matter, which are crucial inputs for supernova and neutron-star calculations. We employ the relativistic mean-field model to describe nuclear interactions. The phase transition from nonuniform matter to uniform matter is determined in a consistent manner. The deconfinement phase transition in neutron-star matter at high densities is examined using the equilibrium conditions derived by minimization of the total free energy.

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“…Again the interaction between a pair of nucleons when they are embedded in a heavy nucleus is less than the force in empty space. This suppression of the two-body interactions within a nucleus in favour of the interaction of each nucleon with the average nucleon density, means that the non-linearity acts as a smoothing mechanism and hence leads in the direction of the one-body potential and shell structure 17,18,19,20 . The replacement of mass term 1 2 m 2 σ σ 2 of σ field by U (σ) and 1 2 m 2 ω V µ V µ of ω field by U (ω).…”

Section: Non-linear Casementioning

confidence: 99%

The Effects of Self Interacting Isoscalar-Vector Meson on Finite Nuclei and Infinite Nuclear Matter

et al. 2015

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A detailed study is made for the nucleon-nucleon interaction based on relativistic mean field theory in which the potential is explicitly expressed in terms of mass and the coupling constant of the meson fields. A unified treatment for self-coupling of isoscalar-scalar σ−, isoscalar-vector ω-mesons and their coupling constant are given with a complete analytic form. The present investigation is focused on the effect of self-interacting higher order σ and ω field on nuclear properties. An attempt is made to explain the collapsing stage of nucleon by higher order ω-field. Both infinite nuclear matter and the finite nuclear properties are included in the present study to observe the behaviour or sensitivity of this self interacting terms.

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Relativistic mean-field theory for unstable nuclei with non-linear σ and ω terms

Cited by 983 publications

References 14 publications

Hot nuclear matter in asymmetry chiral sigma model

Hot nuclear matter in asymmetry chiral sigma model

Finite-Size Effects on Equation of State for Supernovae and Neutron Stars

The Effects of Self Interacting Isoscalar-Vector Meson on Finite Nuclei and Infinite Nuclear Matter

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