Strangeness in nuclei and neutron stars: a challenging puzzle

Strangeness in nuclei and neutron stars: a challenging puzzle

Diego Lonardoni    Alessandro Lovato    Stefano Gandolfi    Francesco Pederiva
Résumé

The prediction of neutron stars properties is strictly connected to the employed nuclear interactions. The appearance of hyperons in the inner core of the star is strongly dependent on the details of the underlying hypernuclear force. We summarize our recent quantum Monte Carlo results on the development of realistic two- and three-body hyperon-nucleon interactions based on the available experimental data for light- and medium-heavy hypernuclei.

Strangeness in nuclei and neutron stars: a challenging puzzle

Diego Lonardoni, Alessandro Lovato, Stefano Gandolfi, et Francesco Pederiva

\@textsuperscript

1Physics Division, Argonne National Laboratory, Lemont, Illinois 60439, USA
\@textsuperscript
2Theoretical Division, Los Alamos National Laboratory, Los Alamos, New Mexico 87545, USA
\@textsuperscript
3Department of Physics, University of Trento, Via Sommarive 14, I-38123 Trento, Italy
\@textsuperscript
4INFN-Trento Institute for Fundamental Physics and Application, Trento, Italy

  • Résumé.

1 Introduction

Neutron stars are among the most compact and dense objects in the Universe, with typical masses up to and radii  km. Their central densities can be several times larger than nuclear saturation density, . At densities larger than , when the nucleon chemical potential is large enough, the conversion of nucleons into hyperons might become energetically favorable, and Pauli blocking would prevent hyperons from decaying by limiting the phase space available to nucleons. This would lead to a reduction of the Fermi pressure exerted by the baryons and to a softening of the equation of state (EOS). As a consequence, the maximum mass determined by the equilibrium condition between gravitational and nuclear forces would be reduced.

Currently there is no general agreement (even qualitative) among the predicted results for the EOS of strange baryonic matter and the maximum mass of a neutron star (NS), that violates the constraints given by the recently measured value of of the millisecond pulsars PSR J1614-2230 [1] and PSR J0348+0432 [2], see Ref. [11]. This apparent inconsistency between NS mass observations and theoretical calculations is a long standing problem known as the hyperon puzzle. It has to be ascribed to a combination of an incomplete knowledge of the forces governing the system and to the concurrent use of approximate theoretical many-body techniques. Its solution requires a more accurate theoretical analysis and a thorough experimental investigation of the hyperon-nucleon force in a variety of systems, ranging from light to medium and heavy hypernuclei.

We employ a quantum Monte Carlo computational technique to tackle the general problem of the hyperon-nucleon interaction. The algorithm, auxiliary field diffusion Monte Carlo (AFDMC), has been introduced by Schmidt and Fantoni [3] as an extension of the usual diffusion Monte Carlo method to deal in an efficient way with spin/isospin-dependent Hamiltonians. It has been successfully applied to solve the many-body problem in a non perturbative fashion for strongly correlated systems, both in the standard [4, 5, 6, 7] and strange nuclear sector [8, 9, 11, 10].

2 Hypernuclei: from few- to many-body systems

As reported in Refs. [8, 9, 10], an accurate analysis of the  separation energy of light- and medium-heavy hypernuclei has been recently carried out using a phenomenological hypernuclear interaction analog to the Argonne-Illinois nucleon-nucleon force [12, 13, 14, 15, 16, 17, 18, 19]. The two-body component of this interaction has been fit to the existing scattering data. The three-body sector instead has been re-fit to the available  separation energies of single- hypernuclei over a wide mass range by means of AFDMC calculations. It has been shown that the repulsive nature of the three-body hyperon-nucleon interaction is the key to satisfactorily reproduce the ground state properties of hypernuclei from light- to medium-heavy within a unique theoretical framework. Fig. 1 shows the AFDMC results for when using the complete force. The agreement with experimental data is good over all the mass range investigated and for the  particle in different single particle states. For more details see Refs. [8, 9, 10].

Figure 1: Measured (see Ref. [10] for the complete list of references) and computed  separation energies as a function of . Results for the  particle in different single particle states are shown.

In the light sector, a two-body charge symmetry breaking interaction has been also employed [13, 9]. As shown in Tab. 1, AFDMC results reproduce the hyperon separation energies and energy splitting of the mirror hypernuclei H and He, according to the old emulsion data [20]. H is weakly bound compared to deuterium and the neutral hypernucleus n is predicted to be unbound, in agreement with other theoretical results [21, 22, 23], contradicting the possible experimental evidence reported in Ref. [24].

System
n  unbound unknown
H  0.23(9) 0.13(5)
H 1.95(9) 2.04(4) 0.42(11) 0.35(6)
He 2.37(9) 2.39(3)
Tableau 1: AFDMC and experimental [20]  separation energies for the lightest hypernuclei. In the case of the separation energy difference is also shown. Evidence for the neutral hypernucleus n has been reported in Ref. [24], but no value has been reported. All energies are in MeV.

In order to validate the phenomenological approach adopted in quantum Monte Carlo calculations for hypernuclei, a benchmark among different few-body methods has been recently proposed. In tab. 2 we report preliminary results for He for two different exact methods, AFDMC and Nonsymmetrized Hyperspherical Harmonics (HSHH) [25]. In both strange and non-strange sectors the employed potentials are at two-body level only. Results agree among different methods whether using a soft (Minnesota [26]) or hard (Argonne V4 [27]) potential.

He AFDMC NSHH
Minn [26] -37.69(8) -37.77(10)
6.95(9) 6.99(10)
AV4 [27] -39.46(12) -39.54(10)
6.70(16) 6.84(10)
Tableau 2: Binding energies and  separation energies for He for different combinations of nucleon-nucleon and hyperon-nucleon potentials and different methods. All energies are in MeV.

3 Neutron stars: from hypernuclei to the infinite medium

Precise AFDMC calculations have been performed to first assess the parameters of the interaction from measured hyperon separation energies, and then to extrapolate the results to the case of neutron matter with strangeness. However, parametrizations of the potential predicting relatively small differences in the  separation energies of hypernuclei give very different results for the properties of the infinite medium [11]. The resulting EOS spans the whole regime extending from the appearance of a substantial fraction of hyperons at to the absence of particles in the entire density range of the star. This yields a sizable effect on the predicted NS structure. Therefore, the derivation of realistic hypernuclear potential models is of paramount importance to properly assess the role of hyperons in NSs and reconcile theoretical predictions with astrophysical observations. This demands a precise and systematic experimental investigation of hypernuclear properties over a wide range of masses. For instance, a recent study of the isospin dependence of the present three-body hyperon-nucleon force shows the difficulty in extracting the information on the Hamiltonian from currently available experimental information on hypernuclei [10].

Remerciements

This work was supported by the U.S. Department of Energy, Office of Science, Office of Nuclear Physics, under the NUCLEI SciDAC grant (D.L., A.L., S.G.), by the Department of Energy, Office of Science, Office of Nuclear Physics, under Contract No. DE-AC02-06CH11357 (A.L.), and by DOE under Contract No. DE-AC52-06NA25396 and Los Alamos LDRD grant (S.G.). This research used resources of the National Energy Research Scientific Computing Center (NERSC), which is supported by the Office of Science of the U.S. Department of Energy under Contract No. DE-AC02-05CH11231, and computing time provided by Institutional Computing (IC) at LANL.

Références

Comments 0
Request Comment
You are adding the first comment!
How to quickly get a good reply:
  • Give credit where it’s due by listing out the positive aspects of a paper before getting into which changes should be made.
  • Be specific in your critique, and provide supporting evidence with appropriate references to substantiate general statements.
  • Your comment should inspire ideas to flow and help the author improves the paper.

The better we are at sharing our knowledge with each other, the faster we move forward.
""
The feedback must be of minimum 40 characters and the title a minimum of 5 characters
   
Add comment
Cancel
Loading ...
242270
This is a comment super asjknd jkasnjk adsnkj
Upvote
Downvote
""
The feedback must be of minumum 40 characters
The feedback must be of minumum 40 characters
Submit
Cancel

You are asking your first question!
How to quickly get a good answer:
  • Keep your question short and to the point
  • Check for grammar or spelling errors.
  • Phrase it like a question
Test
Test description