On the localization of Rydberg wave packets

Chatterjee, Supriya; Saha, Asit; Talukdar, B.

doi:10.1140/epjd/e2013-40103-9

Cited by 22 publications

(28 citation statements)

References 31 publications

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“…This is somewhat surprising since Eq. (11) indicates that the triplet interaction should dominate and since Λ-Σ conversion is stronger for the triplet in most interactions. For NLO19 and Jülich '04, the 1 + state has a larger Σ-probability which is more in line with naive expectations.…”

Section: Three-and Four-body Systemsmentioning

confidence: 99%

“…for ρ in the order of two-to-three times that of normal nuclear matter [10]. For such an interaction the onset for hyperon formation in neutron stars could be shifted to rather high densities, a feature that appears to be promising as a possible explanation for the so-called hyperon puzzle [11]. The latter refers to the still unsolved question how one can reconcile the softening of the equation-of-state due to the appearance of hyperons with the observed large size (mass) of neutron stars [11][12][13][14].…”

Section: Introductionmentioning

confidence: 99%

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Hyperon–nucleon interaction within chiral effective field theory revisited

2020

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The ΛN and ΣN interactions are considered at next-to-leading order in SU(3) chiral effective field theory. Different options for the low-energy constants that determine the strength of the contact interactions are explored. Two variants are analysed in detail which yield equivalent results for ΛN and ΣN scattering observables but differ in the strength of the ΛN → ΣN transition potential. The influence of this difference on predictions for light hypernuclei and on the properties of the Λ and Σ hyperons in nuclear matter is investigated and discussed. The effect of the variation in the potential strength of the ΛN -ΣN coupling (also called Λ − Σ conversion) is found to be moderate for the considered 3 Λ H and 4 Λ He hypernuclei but sizable in case of the matter properties. Further, the size of three-body forces and their relation to different approaches to hypernuclear interactions is discussed.PACS. 12.39.Fe Chiral Lagrangians -13.75.Ev Hyperon-nucleon interactions -21.30.Fe Forces in hadronic systems and effective interactions

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Section: Three-and Four-body Systemsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Hyperon–nucleon interaction within chiral effective field theory revisited

2020

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“…One of the longstanding open problems in nuclear physics and astrophysics that could be (if not completely at least partially) solved with the help of hy-peronic three-body forces (YTBF) is the so-called "hyperon-puzzle" of neutron stars [21,22], i.e., the difficulty to reconcile the measured masses of neutron stars with the presence of hyperons in their interiors. Hyperons are expected to appear at 2 − 3 times normal nuclear saturation density (n 0 = 0.16 fm −3 ).…”

Section: Introductionmentioning

confidence: 99%

Impact of chiral hyperonic three-body forces on neutron stars

Logoteta¹,

Vidaña²,

Bombaci³

2019

Eur. Phys. J. A

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We study the effect of the nucleon-nucleon-lambda (NNΛ) three-body force on neutron stars. In particular, we consider the NNΛ force recently derived by the Jülich-Bonn-Munich group within the framework of chiral effective field theory at next-to-next-to-leading order. This force, together with realistic nucleon-nucleon, nucleon-nucleon-nucleon and nucleon-hyperon interactions, is used to calculate the equation of state and the structure of neutron stars within the many-body non-relativistic Brueckner-Hartree-Fock approach. Our results show that the inclusion of the NNΛ force leads to an equation of state stiff enough such that the resulting neutron star maximum mass is compatible with the largest currently measured (∼ 2 M ⊙ ) neutron star masses. Using a perturbative many-body approach we calculate also the separation energy of the Λ in some hypernuclei finding that the agreement with the experimental data improves for the heavier ones when the effect of the NNΛ force is taken into account.

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“…Nevertheless, due to the large value of the density, new degrees of freedom are expected to appear in addition to nucleons. Examples of these new degrees of freedom widely studied include pion (Haensel & Proszynski (1982)) and kaon (Kaplan & Nelson (1986)) condensates, hyperons (Chatterjee & Vidaña (2016); Vidaña (2018)), ∆ isobars (Drago et al (2014b,a); Ribes et al (2019)), deconfined quarks (Glendenning (1992)) or even di-baryonic matter (Faessler et al (1998)). The most precise and stringent neutron star constraint on the nuclear EoS comes from the recent determination of the unusually high masses of the millisecond pulsars PSR J1614-2230 (Demorest et al (2010)), PSR J0348+0432 (Antoniadis et al (2013)) and PSR J0740+6620 (Cromartie et al (2020)).…”

Section: Introductionmentioning

confidence: 99%

“…This observational constraint rules out many of the existent EoS models with exotic degrees of freedom, although their presence in the neutron star interior is, however, energetically favorable. This has lead to puzzles like the "hyperon puzzle" (Chatterjee & Vidaña (2016)) or the "∆"puzzle (Drago et al (2014b,a)) whose solutions are not easy and presently are subject of very active research.…”

Section: Introductionmentioning

confidence: 99%

Neutron star matter equation of state including d^*-hexaquark degrees of freedom

Mantziris

Pastore

Vidaña³

et al. 2020

A&A

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We present an extension of a previous work where, assuming a simple free bosonic gas supplemented with a relativistic meand field model to describe the pure nucleonic part of the EoS, we studied the consequences that the first non-trivial hexaquark d * (2380) could have on the properties of neutron stars. Compared to that exploratory work we employ a standard non-linear Walecka model including additional terms that describe the interaction of the d * (2380) di-baryon with the other particles of the system through the exchange of σand ω-meson fields. Our results have show that the presence of the d * (2380) leads to maximum masses compatible with the recent observations of ∼ 2M ⊙ millisecond pulsars if the interaction of the d * (2380) is slightly repulsive or the d * (2380) does not interacts at all. An attractive interaction makes the equation of state too soft to be able to support a 2M ⊙ neutron star whereas an extremely repulsive one induces the collapse of the neutron star into a black hole as soon as the d * (2380) appears.

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On the localization of Rydberg wave packets

Cited by 22 publications

References 31 publications

Hyperon–nucleon interaction within chiral effective field theory revisited

Hyperon–nucleon interaction within chiral effective field theory revisited

Impact of chiral hyperonic three-body forces on neutron stars

Neutron star matter equation of state including d^*-hexaquark degrees of freedom

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On the localization of Rydberg wave packets

Cited by 22 publications

References 31 publications

Hyperon–nucleon interaction within chiral effective field theory revisited

Hyperon–nucleon interaction within chiral effective field theory revisited

Impact of chiral hyperonic three-body forces on neutron stars

Neutron star matter equation of state including d*-hexaquark degrees of freedom

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Product

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Neutron star matter equation of state including d^*-hexaquark degrees of freedom