Three-neutron resonance trajectories for realistic interaction models

Lazauskas, Rimantas; Carbonell, J.

doi:10.1103/physrevc.71.044004

Cited by 84 publications

(157 citation statements)

References 35 publications

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“…We should point out that this pole trajectory is similar to that of the three neutron case, but the scaling factor is quite different [16]. In particular, for the three neutron system, where the Pauli exclusion principle plays a significant role, one needs a substantial scaling factor to generate a resonance.…”

Section: Potential Resonances In the λNn Systemmentioning

confidence: 99%

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Resonances in theΛnnsystem

Afnan

Gibson

2015

Phys. Rev. C

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Background: A bound state of the Λnn system has been reported, but at least three theoretical papers question the existence of such a bound state.Purpose: We address the alternative question of whether there might exist a resonance in the Λnn system, using a rank one separable potential formulation of the Hamiltonian. Methods:We examine the eigenvalues of the kernel of the Faddeev equation in the complex energy plane using contour rotation to allow us to analytically continue the kernel onto the second energy sheet. The model Λn interaction is fitted to the Λp scattering length and effective range. Results:We follow the largest eigenvalue as the Λn potentials are scaled and the Λnn continuum is turned first into a resonance, and then into a bound state of the system. Conclusions:Because a change in the strength of the Λn potential of as little as 5% will produce a Λnn resonance, we infer that an experiment of the 3 H(e,e'K + ) 3 Λ n type at JLAB could be used to constrain the properties of the Λn interaction.

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Section: Potential Resonances In the λNn Systemmentioning

confidence: 99%

“…Because resonances lie on the second energy sheet, we need to analytically continue Eqs. (15) and (16) …”

Section: Potential Resonances In the λNn Systemmentioning

confidence: 99%

Resonances in theΛnnsystem

Afnan

Gibson

2015

Phys. Rev. C

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“…The present work confirms previous calculations by the Grenoble and Pisa groups (second and third lines respectively) compiled in ref. [6] together with the results by one of us (fourth line) where the AV18 interaction was represented in rank one. The small differences between the phases in the first three lines are probably due to higher NN partial waves (I ≤ 4) that are included in the present calculation together with ℓ y , ℓ z ≤ 4.…”

Section: Resultsmentioning

confidence: 99%

“…These problems persist even when the Coulomb interaction is added [1,2,3] and seem to be insensitive to the choice of realistic 2N + 3N force model. As it has already been highlighted in the past [4,5,6], the four-nucleon scattering problem reveals further discrepancies between theory and experiment that need clarification in terms of improved calculations using modern force models and efficient numerical algorithms that allow for a numerically converged solution of the Alt, Grassberger and Sandhas (AGS) equation [7] for the transition operators.…”

Section: Introductionmentioning

confidence: 99%

Four-nucleon scattering: a new numerical approach

Deltuva

Fonseca

2007

Nuclear Physics A

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The AGS equations are solved for n 3 H and p 3 He scattering including the Coulomb interaction. Comparison with previous work confirms the accuracy of the calculation and helps clarify a number of issues related to the n 3 H total cross section at the peak of the resonance region, as well as an A y deficiency in p 3 He. Calculations are fully converged in terms of NN partial waves and involve no uncontrolled approximations.

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“…For symmetric nuclear matter (number of protons is equal to the number of neutrons) the energy per particle is approximately equal 16 MeV and the nuclear density is is ρ 0.16 fm −3 [5]. Nuclei that are composed solely from neutrons are believed to have positive energy, however, the question of existence of bound state of N neutrons, where N is large, is still not ultimately resolved [6,7]. When one adds to the interaction also the gravitational forces the neutrons can form neutron stars, which contain nearly 10 57 neutrons.…”

Section: Introductionmentioning

confidence: 99%

Argonne potential and multi-neutron systems

Gridnev

Schramm

Gridnev

et al. 2014

AIP Conference Proceedings

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Abstract. Recently it was proved that the neutron matter interacting through Argonne V18 pair-potential plus modern variants of Urbana or Illinois three-body forces is unstable. For the energy of N neutrons E(N), which interact through these forces one has E(N) = −cN 3 + O(N 8/3 ), where c > 0 is a constant. This means that: (i) the energy per particle and neutron density diverge rapidly for large neutron numbers; (ii) bound states of N neutrons exist for N large enough. The neutron matter collapse is possible due to the form of the repulsive core in three-body forces, which vanishes when three nucleons occupy the same site in space. The obtained results partly change the paradigm, in which the stability of neutron stars is attained through the Pauli principle; the strong repulsive core in the nucleon interactions is by no means less important.

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Three-neutron resonance trajectories for realistic interaction models

Cited by 84 publications

References 35 publications

Resonances in theΛnnsystem

Resonances in theΛnnsystem

Four-nucleon scattering: a new numerical approach

Argonne potential and multi-neutron systems

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