Binding energies of hypernuclei and three-body<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mi>Λ</mml:mi><mml:mi mathvariant="normal">NN</mml:mi></mml:math>forces

Bodmer, A.R.; Usmani, Q. N.; Carlson, J.

doi:10.1103/physrevc.29.684

Cited by 74 publications

(76 citation statements)

References 21 publications

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“…This, however, should not be expected as the Fermi-momentum -if well defined at all in these light systems -should be somewhat different for these hypernuclei. Nevertheless, we like to point out that our calculations do not show the strong overbinding of 5AHe as encountered in previous studies [2,15,16]. In contrast, if we again assume a linear dependence of the BA-value on kF, a static approach, in which we use the Yamamoto-Bando AN-interaction with a common value for the parameter k F for all s-shell hypernuclei, shows the strong overbinding of the 5AHe hypernucleus compared to the other s-shell hypernuclei.…”

Section: Distortion Effects In the S-sheu Hypernucleimentioning

confidence: 76%

Distortion effects in light hypernuclei

Warmann

Langanke

1989

Z. Physik A - Atomic Nuclei

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We have studied the particle-bound levels in the hypernuclei 3A'4H, ]He, ]Li and 8'9Be in the framework of the full microscopic Resonating Group Method (RGM). In a first step we have solved the respective nuclear many-body problem within the RGM. For each hypernucleus we have then performed a static calculation, in which the nuclear degrees of freedom were kept fixed, and a dynamical calculation in which nuclear degrees of freedom were allowed to vary. The differences between these two studies allowed us to investigate nuclear distortion effects caused by the presence of the A-particle. We find the nuclear distortion effects to be inverse proportional to the binding of the nuclear constituents. Thus, the strongest effects are observed for 3aH and for 9aBe. Our dynamical approach does not show the strong overbinding of 5aHe and 9Be as reported in other cluster model studies. Our results for the p-shell hypernuclei agree reasonably well with those obtained in a semi-microscopic Orthogonal Condition Model (OCM) study which used the same effective AN-interaction as employed in our calculation.

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Section: Distortion Effects In the S-sheu Hypernucleimentioning

confidence: 76%

Distortion effects in light hypernuclei

Warmann

Langanke

1989

Z. Physik A - Atomic Nuclei

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“…The latest version of the Argonne potential (Wiringa, Stoks, and Schiavilla, 1995), called v 18 , not only contains isoscalar operators but includes an electromagnetic part and isovector operators such that the charge dependence of the NN force is successfully described. Also, some models with Λ hyperons are available, but they are much less sophisticated due to the small amount of hyperonic data; see, e.g., Bodmer, Usmani, and Carlson (1984).…”

Section: B Potential Modelsmentioning

confidence: 99%

Equations of state for supernovae and compact stars

et al. 2017

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A review is given of various theoretical approaches for the equation of state (EoS) of dense matter, relevant for the description of core-collapse supernovae, compact stars, and compact star mergers. The emphasis is put on models that are applicable to all of these scenarios. Such EoS models have to cover large ranges in baryon number density, temperature, and isospin asymmetry. The characteristics of matter change dramatically within these ranges, from a mixture of nucleons, nuclei, and electrons to uniform, strongly interacting matter containing nucleons, and possibly other particles such as hyperons or quarks. As the development of an EoS requires joint efforts from many directions, different theoretical approaches are considered and relevant experimental and observational constraints which provide insights for future research are discussed. Finally, results from applications of the discussed EoS models are summarized.

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“…during the early days of hypernuclear physics, as an important ingredient to calculate the binding energy of hypernuclei. Since then the ΛNN interaction received considerable attention in many other studies of hypernuclei [35][36][37][38][39][40][41][42][43]. It is thus quite natural to expect that YTBIs can influence the EoS of dense matter and can represent a likely candidate to solve the hyperon puzzle [45][46][47][48].…”

Section: Hyperon Starsmentioning

confidence: 99%

The Hyperon Puzzle in Neutron Stars

Bombaci

2017

Proceedings of the 12th International Conference on Hypernuclear and Strange Particle Physics (HYP2015)

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The so called hyperon puzzle, i.e. the difficulty to reconcile the measured masses of neutron stars (NSs) with the presence of hyperons in their interiors, is one of the hot topics in astrophysics which is stimulating copious experimental and theoretical research in hypernuclear physics. After illustrating the origin of the hyperon puzzle, I discuss some of its possible solutions, and particularly those related to the role of hyperonic two-and three-body interactions on the equation of state of dense matter. Afterward, I discuss a possibility to circumvent the hyperon puzzle allowing for the presence of strangeness in NSs in the form of deconfined strange quark matter, and thus considering the so called quark stars, i.e. hybrid stars or strange stars. Finally I discuss the astrophysical consequences of the possible conversion process of an hadronic star to a quark star.

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Binding energies of hypernuclei and three-bodyΛNNforces

Cited by 74 publications

References 21 publications

Distortion effects in light hypernuclei

Distortion effects in light hypernuclei

Equations of state for supernovae and compact stars

The Hyperon Puzzle in Neutron Stars

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