dorsal/arxiv
View SchemaEffects of $\omega$ meson self-coupling on the properties of finite nuclei and neutron stars
| Authors | Raj Kumar, B. K. Agrawal, Shashi K. Dhiman |
|---|---|
| Categories | |
| ArXiv ID | nucl-th/0608034 |
| URL | https://arxiv.org/abs/nucl-th/0608034 |
| DOI | 10.1103/PhysRevC.74.034323 |
| Journal | Phys.Rev.C74:034323,2006 |
Abstract
The effects of $\omega$ meson self-coupling (OMSC) on the properties of finite nuclei and neutron stars are investigated within the framework of effective field theory based relativistic mean-field (ERMF) model which includes the contributions from all possible mixed interactions between the scalar-isoscalar ($\sigma$), vector-isoscalar ($\omega$) and vector-isovector ($\rho$) mesons upto the quartic order. For a realistic investigation, several parameter sets corresponding to different values of OMSC are generated by adjusting the remaining parameters of the ERMF model to fit the properties of the finite nuclei. Though, all these parameter sets give equally good fit to the properties of the finite nuclei, only moderate values of OMSC are favored from the "naturalness" point of view. The equation of state for the symmetric nuclear and pure neutron matters resulting from the parameter sets with the moderate values of OMSC are in close agreement with the ones obtained within the Dirac-Brueckner-Hartree-Fock approximation. For such parameter sets the limiting mass for the neutron stars composed of $\beta$-stable matter is $\sim 1.9M_\odot$. It is found that the direct Urca process can occur in the neutron stars with "canonical" mass of $1.4M_\odot$ only for the moderate and higher values of OMSC. Some other interesting properties for the neutron stars are also discussed.
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"abstract": "The effects of $\\omega$ meson self-coupling (OMSC) on the properties of\nfinite nuclei and neutron stars are investigated within the framework of\neffective field theory based relativistic mean-field (ERMF) model which\nincludes the contributions from all possible mixed interactions between the\nscalar-isoscalar ($\\sigma$), vector-isoscalar ($\\omega$) and vector-isovector\n($\\rho$) mesons upto the quartic order. For a realistic investigation, several\nparameter sets corresponding to different values of OMSC are generated by\nadjusting the remaining parameters of the ERMF model to fit the properties of\nthe finite nuclei. Though, all these parameter sets give equally good fit to\nthe properties of the finite nuclei, only moderate values of OMSC are favored\nfrom the \"naturalness\" point of view. The equation of state for the symmetric\nnuclear and pure neutron matters resulting from the parameter sets with the\nmoderate values of OMSC are in close agreement with the ones obtained within\nthe Dirac-Brueckner-Hartree-Fock approximation. For such parameter sets the\nlimiting mass for the neutron stars composed of $\\beta$-stable matter is $\\sim\n1.9M_\\odot$. It is found that the direct Urca process can occur in the neutron\nstars with \"canonical\" mass of $1.4M_\\odot$ only for the moderate and higher\nvalues of OMSC. Some other interesting properties for the neutron stars are\nalso discussed.",
"arxiv_id": "nucl-th/0608034",
"authors": [
"Raj Kumar",
"B. K. Agrawal",
"Shashi K. Dhiman"
],
"categories": [
"nucl-th"
],
"doi": "10.1103/PhysRevC.74.034323",
"journal_ref": "Phys.Rev.C74:034323,2006",
"title": "Effects of $\\omega$ meson self-coupling on the properties of finite nuclei and neutron stars",
"url": "https://arxiv.org/abs/nucl-th/0608034"
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