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

Biswal, S. K.; Singh, Shailesh Kumar; Bhuyan, M.; Patra, S. K.

doi:10.1007/s13538-015-0317-z

Cited by 9 publications

(7 citation statements)

References 35 publications

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“…A detailed account on the importance of various couplings can be obtained in Refs. [2,22,23,24]. The parameters, such as η 1 , η 2 , η 2ρ , α 1 , α 2 , f ω have their own importance to explain various properties of finite nuclei and nuclear matter.…”

Section: Resultsmentioning

confidence: 99%

New parameterization of the effective field theory motivated relativistic mean field model

et al. 2017

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A new parameter set is generated for finite and infinite nuclear system within the effective field theory motivated relativistic mean field (ERMF) formalism. The isovector part of the ERMF model employed in the present study includes the coupling of nucleons to the δ and ρ mesons and the cross-coupling of ρ mesons to the σ and ω mesons. The results for the finite and infinite nuclear systems obtained using our parameter set are in harmony with the available experimental data. We find the maximum mass of the neutron star to be 2.03M ⊙ and yet a relatively smaller radius at the canonical mass, 12.69 km, as required by the available data.

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Section: Resultsmentioning

confidence: 99%

New parameterization of the effective field theory motivated relativistic mean field model

et al. 2017

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“…In the case of IOPB-I, there are two extra coupling parameters, Λ ω and ζ 0 are taken on top of the NL3 parameter set. These two coupling parameters play a vital role in both finite and infinite NM system (Singh et al 2014;Biswal et al 2015;Kumar et al 2018). The parameter Λ ω controls the symmetry energy (or neutron skin thickness of finite nuclei) as well as the maximum mass of the NS (Horowitz & Piekarewicz 2001).…”

Section: Choice Of Parameter Setsmentioning

confidence: 99%

Effects of dark matter on the nuclear and neutron star matter

Das

Kumar

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We study the dark matter (DM) effects on the nuclear matter (NM) parameters characterizing the equation of states of super dense neutron-rich nucleonic matter. The observables of the NM, i.e. incompressibility, symmetry energy and its higher order derivatives in the presence DM for symmetric and asymmetric NM are analysed with the help of an extended relativistic mean field model. The calculations are also extended to β-stable matter to explore the properties of the neutron star (NS). We analyse the DM effects on symmetric NM, pure neutron matter, and NS using NL3, G3, and IOPB-I forces. The binding energy per particle and pressure is calculated with and without considering the DM interaction with the NM systems. The influences of DM are also analysed on the symmetry energy and its different coefficients. The incompressibility and the skewness parameters are affected considerably due to the presence of DM in the NM medium. We extend the calculations to the NS and find its mass, radius and the moment of inertia for static and rotating NS with and without DM contribution. The mass of the rotating NS is considerably changing due to rapid rotation with the frequency in the mass-shedding limit. The effects of DM are found to be important for some of the NM parameters, which are crucial for the properties of astrophysical objects.

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“…These both sets have positive k 3 and negative k 4 corresponding to cubic and quartic terms arising from the self couplings of the σ meson. It is to be noted that a large negative value of k 4 leads to the divergence of a solution in the lighter mass region of the periodic table [50]. The scalar and vector cross-couplings η 1 and η 2 zero in these sets are zero yet they have the value of vector self-coupling ζ 0 within the acceptable limit.…”

Section: Force Parametersmentioning

confidence: 94%

Critical properties of symmetric nuclear matter in low-density regime using effective-relativistic mean field formalism

Parmar¹,

Sharma²,

Patra³

2021

J. Phys. G: Nucl. Part. Phys.

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The effective field theory motivated relativistic mean-field (E-RMF) formalism is employed to study the equation of state (EoS) for the infinite symmetric nuclear matter (SNM) at finite temperature using the recently developed forces FSUGarnet, IOPB-I, G3, and the well known NL3 force parameter. The EoS is then used to estimate the critical temperature T c, pressure P c and density ρ c of the SNM for the liquid–gas phase transition. As T c is not a constrained parameter in both experiments and theoretical calculations, there is a large uncertainty around its value. Although, the critical parameters are correlated among themselves. It is revealed that vector self-coupling ζ 0 of used forces play determining role in EoS in finite temperature limit. Keeping the incompressibility in acceptable limit i.e. 240 ± 20 MeV, the lower value of ζ 0 gives a better result of T c when compared to the several experimental data. The critical parameters however show weak correlation with the properties at saturation density at zero temperature. The compressibility factors calculated with these parameters are in agreement with the universal value of liquid–gas systems. Stability conditions are examined along with binodal and spinodal regions. Besides this, the thermodynamic properties like specific heat and latent heat are also worked out. We have carried out detailed consistency check of our calculations using critical exponents and standard scaling laws. All the exponents are well within the theoretical mean-field results.

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

Cited by 9 publications

References 35 publications

New parameterization of the effective field theory motivated relativistic mean field model

New parameterization of the effective field theory motivated relativistic mean field model

Effects of dark matter on the nuclear and neutron star matter

Critical properties of symmetric nuclear matter in low-density regime using effective-relativistic mean field formalism

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