Large-Mass Neutron Stars With Hyperonization

Jiang, Wei-Zhou; Li, Bao-An; Chen, Lie‐Wen

doi:10.1088/0004-637x/756/1/56

Cited by 70 publications

(31 citation statements)

References 68 publications

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“…It is our future subject to show that our stiff EoS with universal MPP repulsions is free from the softening effect induced by hyperon mixing to neutron-star matter. Such a work will be complementary to the analyses based on the relativistic mean field models [19][20][21] for a massive neutron star including hyprons.…”

Section: Discussionmentioning

confidence: 99%

Multi-Pomeron repulsion and the neutron-star mass

et al. 2013

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A multi-pomeron exchange potential (MPP) is proposed as a model for the three-body repulsion indicated in neutron-star matter, which works universally among three-and four-baryons. Its strength is determined by analyzing the nucleus-nucleus scattering with the G-matrix folding model. The EoS in neutron matter is obtained including the MPP contribution. The neutron-star mass is calculated by solving the TOV equation. The maximum mass is obtained to be larger than the observed one 1.97M solar on the basis of the experimental data.

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Section: Discussionmentioning

confidence: 99%

Multi-Pomeron repulsion and the neutron-star mass

et al. 2013

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“…In order to keep the background from bremsstrahlung low we focus for the production of light hyperfragments on low Z targets like 12 C, 9 Be and natural 6,7 Li. In the 2011 and 2012 experiments a 22 mg/cm 2 thick beryllium foil was bombarded by a 1.5 GeV electron beam.…”

Section: Decay Pion Spectroscopy At Mamimentioning

confidence: 99%

“…[2] and references therein). However, our limited knowledge of the hyperon-nucleon, the hyperon-hyperon and the three-body YNN or YYN interactions and possible charge symmetry breaking in these interactions [3] still does not rule out the appearance of hyperons in the inner core of neutron stars [4,5,6,7,8]. Indeed the presence of hyperons may not only show up in the neutron star mass but can also play a crucial role in the dynamics of the core-collapse supernovae or in neutron star mergers [9].…”

Section: Introductionmentioning

confidence: 99%

“…Thus nucleon-nucleon interactions from χEFT Hypernuclei showing two-body pionic decays and which are accessible by high precision pion spectroscopy using a 7 Li (light grey background), 9 Be (grey) and 12 C target (black). Already with 7 Li and 9 Be targets all isobars with A=6 can be studied. Right: Relative probabilities of hyperfragment production predicted by a statistical decay model [14] for a primary 9 Λ Li nucleus as a function of its excitation energy.…”

Section: Introductionmentioning

confidence: 99%

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High precision mass measurements of hypernuclei - achievements and perspectives

Pochodzalla¹

2013

Proceedings of XTH Quark Confinement and the Hadron Spectrum — PoS(Confinement X)

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At the Mainz Microtron MAMI hypernuclei can be produced by (e,e K) reactions. A dedicated kaon spectrometer positioned at 0 • with respect to the incident electron beam is used to tag events involving strangeness production. By measuring the momenta of pions from two body weak decays one gains direct access to the ground state masses of the produced hyperfragments. In this contribution the motivation of the experiment and the experimental challenges are presented. PoS(Confinement X)254High precision mass measurements of hypernuclei -achievements and perspectives J. PochodzallaThe twofold way Direct production spectroscopy Examples strangeness production missing massDecay spectroscopy γ-decay of excited states π from weak decay charged fragments Examples nuclear emulsions heavy ion reactions antiproton induced reactions continuum excitation in (e,e´K + )Figure 1: Two classes of reactions to produce and study hypernuclei. Missing mass spectroscopy which employs kinematic information of the production process (left) and the decay spectroscopy which relies on the detection of the decay products (right). At MAMI hypernuclei are produced in (e,e K + ) reactions. Pions from the weak decay of deexcited hyperfragments are used to identify the hypernuclei.

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“…[20] proposed an EoS with maximum mass ∼ 2.1M ⊙ using the quark-meson coupling model, which naturally incorporates hyperons without additional parameters. A model with in-medium hyperon interactions is considered in [21].…”

Section: Introductionmentioning

confidence: 99%

Magnetic neutron stars in f(R) gravity

Astashenok

Capozziello

Odintsov

2014

Astrophys Space Sci

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Neutron stars with strong magnetic fields are considered in the framework of f (R) gravity. In order to describe dense matter in magnetic field, the model with baryon octet interacting through σρω-fields is used. The hyperonization process results in softening the equation of state (EoS) and in decreasing the maximal mass. We investigate the effect of strong magnetic field in models involving quadratic and cubic corrections in the Ricci scalar R to the Hilbert-Einstein action. For large fields, the Mass-Radius relation differs considerably from that of General Relativity only for stars with masses close to the maximal one. Another interesting feature is the possible existence of more compact stable stars with extremely large magnetic fields (∼ 6 × 10 18 G instead of ∼ 4 × 10 18G as in General Relativity) in the central regions of the stars. Due to cubic terms, a significant increasing of the maximal mass is possible.

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Large-Mass Neutron Stars With Hyperonization

Cited by 70 publications

References 68 publications

Multi-Pomeron repulsion and the neutron-star mass

Multi-Pomeron repulsion and the neutron-star mass

High precision mass measurements of hypernuclei - achievements and perspectives

Magnetic neutron stars in f(R) gravity

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