Relativistic effective interaction for nuclei, giant resonances, and neutron stars

Fattoyev, F. J.; Horowitz, C. J.; Piekarewicz, J.; Shen, Gang

doi:10.1103/physrevc.82.055803

Cited by 336 publications

(352 citation statements)

References 45 publications

Supporting

Mentioning

338

Contrasting

Unclassified

Order By: Relevance

“…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%

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

Fattoyev

Piekarewicz

2011

Phys. Rev. C

Self Cite

View full text Add to dashboard Cite

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%.

show abstract

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

Self Cite

View full text Add to dashboard Cite

show abstract

“…This approach has been successfully used to shape new functionals (see, e.g., Refs. [11][12][13][14][15][16]). In this work, we study the neutron polaron and use its energy as a constraint on nuclear density functionals.…”

mentioning

confidence: 99%

Neutron polaron as a constraint on nuclear density functionals

et al. 2014

View full text Add to dashboard Cite

We study the energy of an impurity (polaron) that interacts strongly in a sea of fermions when the effective range of the impurity-fermion interaction becomes important, thereby mapping the Fermi polaron of condensed matter physics and ultracold atoms to strongly interacting neutrons. We present Quantum Monte Carlo results for this neutron polaron, and compare these with effective field theory calculations that also include contributions beyond the effective range. We show that stateof-the-art nuclear density functionals vary substantially and generally underestimate the neutron polaron energy. Our results thus provide constraints for adjusting the time-odd components of nuclear density functionals to better characterize polarized systems. Energy-density functionals are the only method available to study heavy nuclei and to globally describe the chart of nuclides [1,2]. Due to the need for a precise description of low-energy observables, parameters of these functionals are generally fit to properties of nuclei, including masses and radii. This empirical construction can therefore also benefit from additional input to constrain their properties in exotic, i.e., neutron-rich or spin-polarized systems. Examples of such pseudo-data include calculations of neutron matter [3-9] and neutron drops [10]. This approach has been successfully used to shape new functionals (see, e.g., Refs. [11-16]). In this work, we study the neutron polaron and use its energy as a constraint on nuclear density functionals.The polaron was first introduced in condensed matter physics, and has recently been investigated in strongly interacting ultracold Fermi gases [17] -a system that has many similarities with the physics of low-density neutron matter (see, e.g., Refs. [3,4]). The Fermi polaron is an impurity interacting in a Fermi sea, realized in ultracold atoms and neutron matter as a spin-down fermion in a sea of N ↑ spin-up fermions. The polaron energy E pol = E N ↑ +1 − E N ↑ is defined as the energy difference between the system with the polaron added and the N ↑ (noninteracting) Fermi system. In the thermodynamic limit, this is equivalent to the spin-down chemical potential in the limit of high polarization, and therefore constrains the phase diagram of strongly interacting Fermi systems as a function of spin imbalance [18][19][20][21][22].For attractive interactions, E pol < 0 measures the polaron binding energy in the Fermi sea. In the unitary limit, where the S-wave scattering length |a| → ∞, the polaron energy is universal at low densities and scales as E pol = ηE F where E F = k 2 F /2m is the Fermi energy (with Fermi momentum k F ) and η < 0 is a universal number [18]. Neutrons, whose scattering length is large (a = −18.5 fm), have low-density properties close to the unitary limit. At unitarity, the polaron energy admits a variational bound that sums one-particle-one-hole excitations, η ≤ −0.6066 [18], which is remarkably close to a full manybody treatment [23], η = −0.6158, and agrees with Quantum Monte Carlo (QMC) calculation...

show abstract

“…For our base models we use two recently established EOSs for neutron-rich nucleonic matter within the IU-FSU Relativistic Mean Field (RMF) and the SkIU-FSU Skyrme-Hartree-Fork (SHF) models [20][21][22]. The slope of the symmetry energy at saturation for these models is L = 47.2 MeV.…”

Section: The Equation Of State Of Nuclear Mattermentioning

confidence: 99%

Shedding Light on the EOS-Gravity Degeneracy and Constraining the Nuclear Symmetry Energy from the Gravitational Binding Energy of Neutron Stars

Fattoyev

et al. 2016

EPJ Web of Conferences

Self Cite

View full text Add to dashboard Cite

Abstract. A thorough understanding of properties of neutron stars requires both a reliable knowledge of the equation of state (EOS) of super-dense nuclear matter and the strong-field gravity theories simultaneously. To provide information that may help break this EOS-gravity degeneracy, we investigate effects of nuclear symmetry energy on the gravitational binding energy of neutron stars within GR and the scalar-tensor subset of alternative gravity models. We focus on effects of the slope L of nuclear symmetry energy at saturation density and the high-density behavior of nuclear symmetry energy. We find that the variation of either the density slope L or the high-density behavior of nuclear symmetry energy leads to large changes in the binding energy of neutron stars. The difference in predictions using the GR and the scalar-tensor theory appears only for massive neutron stars, and even then is significantly smaller than the difference resulting from variations in the symmetry energy.

show abstract

Relativistic effective interaction for nuclei, giant resonances, and neutron stars

Cited by 336 publications

References 45 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

Neutron polaron as a constraint on nuclear density functionals

Shedding Light on the EOS-Gravity Degeneracy and Constraining the Nuclear Symmetry Energy from the Gravitational Binding Energy of Neutron Stars

Contact Info

Product

Resources

About