New parametrization for the Lagrangian density of relativistic mean field theory

Lalazissis, G. A.; Konig, Joshua Leon; Ring, P.

doi:10.1103/physrevc.55.540

Cited by 1,670 publications

(2,171 citation statements)

References 29 publications

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“…Such a problem was successfully solved by Boguta and Bodmer with the introduction of cubic and quartic scalar meson self-interactions [15]. Remarkably, using only these six parameters (m s , g s , g v , g ρ , κ, λ) it is possible to reproduce a host of ground-state properties of finite nuclei (both spherical and deformed) throughout the periodic table [16,17]. And by adding two additional parameters (ζ and Λ v ) the success of the model can be extended to the realm of nuclear collective excitations and neutron-star properties [18][19][20][21].…”

Section: A Relativistic Mean-field Modelsmentioning

confidence: 99%

“…In principle then, all model parameters must be retained and subsequently determined from a fit to empirical data. In practice, however, many successful theoretical models-such as NL3 [16,17] and FSUGold [19]-arbitrarily set some of these parameters to zero. The "justification" behind these fairly ad-hoc procedure is that whereas the neglected terms are of the same order in a power-counting scheme, the full set of parameters is poorly determined by existing data, so ignoring a subset model parameters does not compromise the quality of the fit [10,22].…”

Section: A Relativistic Mean-field Modelsmentioning

confidence: 99%

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Accurate calibration of relativistic mean-field models: Correlating observables and providing meaningful theoretical uncertainties

Fattoyev

Piekarewicz

2011

Phys. Rev. C

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Theoretical uncertainties in the predictions of relativistic mean-field models are estimated using a chi-square minimization procedure that is implemented by studying the small oscillations around the chi-square minimum. By diagonalizing the matrix of second derivatives, one gains access to a wealth of information-in the form of powerful correlations-that would normally remain hidden. We illustrate the power of the covariance analysis by using two relativistic mean-field models: (a) the original linear Walecka model and (b) the accurately calibrated FSUGold parametrization. In addition to providing meaningful theoretical uncertainties for both model parameters and predicted observables, the covariance analysis establishes robust correlations between physical observables. In particular, we show that whereas the correlation coefficient between the slope of the symmetry energy and the neutron-skin thickness of Lead is indeed very large, a 1% measurement of the neutron radius of Lead may only be able to constrain the slope of the symmetry energy to about 30%.

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Section: A Relativistic Mean-field Modelsmentioning

confidence: 99%

Section: A Relativistic Mean-field Modelsmentioning

confidence: 99%

Accurate calibration of relativistic mean-field models: Correlating observables and providing meaningful theoretical uncertainties

Fattoyev

Piekarewicz

2011

Phys. Rev. C

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“…In these two last figures we only want to exhibit the correlations between the incompressibility and the effective nucleon mass on one hand and the saturation density on the other. The specific values of the two first quantities are not important here and we would certainly get more reasonable results for them at the nuclear matter saturation density had we used the nonlinear Walecka model [15]. …”

Section: Resultsmentioning

confidence: 96%

“…This model with a very limited number of parameters is also able to describe deformed nuclei [11,12] and for the first time the anomalous shifts in the isotopic chains of different nuclei has been explained [13,14]. As a consequence of all this work, a new parametrization for this non-linear version of the Walecka model has been proposed and gives a very good description not only for the properties of stable nuclei but also for the nuclei far from the valley of beta stability [15].…”

Section: Introductionmentioning

confidence: 99%

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The Coester line in relativistic mean field nuclear matter

Delfino¹,

Malheiro²,

Timóteo³

et al. 2005

Braz. J. Phys.

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The Walecka model contains essentially two parameters that are associated with the Lorentz scalar (S) and vector (V ) interactions. These parameters are related to a two-body interaction consisting of S and V , imposing the condition that the two-body binding energy is fixed. We have obtained a set of different values for the nuclear matter binding energies (BN ) at equilibrium densities (ρo). We investigated the existence of a linear correlation between B N and ρ o , claimed to be universal for nonrelativistic systems and usually known as the Coester line, and found an approximate linear correlation only if V − S remains constant. It is shown that the relativistic content of the model, which is related to the strength of V − S , is responsible for the shift of the Coester line to the empirical region of nuclear matter saturation.

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Reinvestigation of the electron fraction and electron Fermi energy of neutron star

et al. 2017

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In this work, we reinvestigate the electron fraction Ye and electron Fermi energy EF(e) of neutron stars, based on our previous work, in which we first deduce a special solution to EF(e), and then obtain several useful analytical formulae for Ye and matter density ρ within classical models and the relativistic mean‐field (RMF) theory using numerical fitting. The advantages of this formalism include the following: (a) Linear functions are substituted for the nonlinear exponential functions used in the previous work. This method may be simpler and closer to realistic equation of state (EoS) of a neutron star (NS) because there are linear or quasi‐linear relationships between number fractions of leptons and matter density, which can be seen by solving NS EoS. (b) We introduce a dimensionless variable ϱ (ϱ = ρ/ρ0, ρ0 is the standard saturated nuclear density), which greatly reduces the scope of the fitting coefficients. (c) We present numerical errors including absolute and relative deviations between the data and fit. By numerical simulations, we obtain several analytical formulae for Ye and ρ for both APR98 and RMF models. Combining these analytical formulae with the special solution, we can calculate the value of EF(e) for any given matter density. Since Ye and EF(e) are important in assessing the cooling rate of an NS and the possibility of kaon/pion condensation in the NS's interior, this formalism could be useful in the future studies on the thermal evolution of an NS.

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New parametrization for the Lagrangian density of relativistic mean field theory

Cited by 1,670 publications

References 29 publications

Accurate calibration of relativistic mean-field models: Correlating observables and providing meaningful theoretical uncertainties

Accurate calibration of relativistic mean-field models: Correlating observables and providing meaningful theoretical uncertainties

The Coester line in relativistic mean field nuclear matter

Reinvestigation of the electron fraction and electron Fermi energy of neutron star

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