Hyperon matter at low densities

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Abstract

It was reported recently that hyperons can be present inside PSRJ1614-2230 compact star. This can be realized only if the strength of the ω-hyperons and φ-hyperons coupling of conventional hyperons coupling constant on the extended relativistic mean field (ERMF) model increase by a factor of 1.5 to 3. In the present work, the mass and radius relation of the neutron star that is calculated by using BSR28 parameter set of ERMF model augmented with maximal coupling strength of the ω-hyperons and φ-hyperons (X=1), is compared to the mass and radius relation of the neutron star that is predicted by the same RMF parameter set but by assuming that hyperons do not exist in the matter (No. Hyp) as well as those by assuming the hyperons coupling constant fulfilled the conventional SU(6) and SU(3) symmetry. The consequences of implementing X=1 prescription are also discussed. The potential depths of hyperons in symmetric nuclear matter (SNM), pure neutron matter (PNM) and pure lambda matter (PLM) based on this parameter set are also calculated by using the X=1, SU (6) and SU (3) prescriptions. The results are compared to those obtained from microscopic models, quark meson coupling model (χ QMM) and the QCD sum rule for finite density (QCD SM) result.

Original languageEnglish
Title of host publicationAIP Conference Proceedings
EditorsMitra Djamal, Nandang Mufti, Markus Diantoro
PublisherAmerican Institute of Physics Inc.
Pages148-151
Number of pages4
ISBN (Electronic)9780735412545
DOIs
Publication statusPublished - 1 Jan 2014
Event3rd International Conference on Theoretical and Applied Physics 2013, ICTAP 2013 - Malang, East Java, Indonesia
Duration: 10 Oct 201311 Oct 2013

Publication series

NameAIP Conference Proceedings
Volume1617
ISSN (Print)0094-243X
ISSN (Electronic)1551-7616

Conference

Conference3rd International Conference on Theoretical and Applied Physics 2013, ICTAP 2013
CountryIndonesia
CityMalang, East Java
Period10/10/1311/10/13

Keywords

  • High density matter
  • Neutron stars
  • Relativistic mean field model

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