Hadron–Quark Phase Transition in the SU (3) Local Nambu–Jona-Lasinio (NJL) Model with Vector Interaction
We study the hadron–quark hybrid equation of state (EOS) of compact-star matter. The Nambu–Jona-Lasinio (NJL) local SU (3) model with vector-type interaction is used to describe the quark matter phase, while the relativistic mean field (RMF) theory with the scalar-isovector <inline-formula><...
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MDPI AG
2021-01-01
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| Online Access: | https://www.mdpi.com/2073-8994/13/1/124 |
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| author | Grigor Alaverdyan |
| author_facet | Grigor Alaverdyan |
| author_sort | Grigor Alaverdyan |
| collection | DOAJ |
| description | We study the hadron–quark hybrid equation of state (EOS) of compact-star matter. The Nambu–Jona-Lasinio (NJL) local SU (3) model with vector-type interaction is used to describe the quark matter phase, while the relativistic mean field (RMF) theory with the scalar-isovector <inline-formula><math display="inline"><semantics><mi>δ</mi></semantics></math></inline-formula>-meson effective field is adopted to describe the hadronic matter phase. It is shown that the larger the vector coupling constant <inline-formula><math display="inline"><semantics><mrow><msub><mi>G</mi><mi>V</mi></msub></mrow></semantics></math></inline-formula>, the lower the threshold density for the appearance of strange quarks. For a sufficiently small value of the vector coupling constant, the functions of the mass dependence on the baryonic chemical potential have regions of ambiguity that lead to a phase transition in nonstrange quark matter with an abrupt change in the baryon number density. We show that within the framework of the NJL model, the hypothesis on the absolute stability of strange quark matter is not realized. In order to describe the phase transition from hadronic matter to quark matter, Maxwell’s construction is applied. It is shown that the greater the vector coupling, the greater the stiffness of the EOS for quark matter and the phase transition pressure. Our results indicate that the infinitesimal core of the quark phase, formed in the center of the neutron star, is stable. |
| first_indexed | 2024-03-09T04:59:57Z |
| format | Article |
| id | doaj.art-509d443ad6fd46e38c717ac91adbd35d |
| institution | Directory Open Access Journal |
| issn | 2073-8994 |
| language | English |
| last_indexed | 2024-03-09T04:59:57Z |
| publishDate | 2021-01-01 |
| publisher | MDPI AG |
| record_format | Article |
| series | Symmetry |
| spelling | doaj.art-509d443ad6fd46e38c717ac91adbd35d2023-12-03T13:00:59ZengMDPI AGSymmetry2073-89942021-01-0113112410.3390/sym13010124Hadron–Quark Phase Transition in the SU (3) Local Nambu–Jona-Lasinio (NJL) Model with Vector InteractionGrigor Alaverdyan0Department of Radio Physics, Yerevan State University, 1 Alex Manoogian Street, Yerevan 0025, ArmeniaWe study the hadron–quark hybrid equation of state (EOS) of compact-star matter. The Nambu–Jona-Lasinio (NJL) local SU (3) model with vector-type interaction is used to describe the quark matter phase, while the relativistic mean field (RMF) theory with the scalar-isovector <inline-formula><math display="inline"><semantics><mi>δ</mi></semantics></math></inline-formula>-meson effective field is adopted to describe the hadronic matter phase. It is shown that the larger the vector coupling constant <inline-formula><math display="inline"><semantics><mrow><msub><mi>G</mi><mi>V</mi></msub></mrow></semantics></math></inline-formula>, the lower the threshold density for the appearance of strange quarks. For a sufficiently small value of the vector coupling constant, the functions of the mass dependence on the baryonic chemical potential have regions of ambiguity that lead to a phase transition in nonstrange quark matter with an abrupt change in the baryon number density. We show that within the framework of the NJL model, the hypothesis on the absolute stability of strange quark matter is not realized. In order to describe the phase transition from hadronic matter to quark matter, Maxwell’s construction is applied. It is shown that the greater the vector coupling, the greater the stiffness of the EOS for quark matter and the phase transition pressure. Our results indicate that the infinitesimal core of the quark phase, formed in the center of the neutron star, is stable.https://www.mdpi.com/2073-8994/13/1/124quark matterNJL modelRMF theorydeconfinement phase transitionMaxwell construction |
| spellingShingle | Grigor Alaverdyan Hadron–Quark Phase Transition in the SU (3) Local Nambu–Jona-Lasinio (NJL) Model with Vector Interaction Symmetry quark matter NJL model RMF theory deconfinement phase transition Maxwell construction |
| title | Hadron–Quark Phase Transition in the SU (3) Local Nambu–Jona-Lasinio (NJL) Model with Vector Interaction |
| title_full | Hadron–Quark Phase Transition in the SU (3) Local Nambu–Jona-Lasinio (NJL) Model with Vector Interaction |
| title_fullStr | Hadron–Quark Phase Transition in the SU (3) Local Nambu–Jona-Lasinio (NJL) Model with Vector Interaction |
| title_full_unstemmed | Hadron–Quark Phase Transition in the SU (3) Local Nambu–Jona-Lasinio (NJL) Model with Vector Interaction |
| title_short | Hadron–Quark Phase Transition in the SU (3) Local Nambu–Jona-Lasinio (NJL) Model with Vector Interaction |
| title_sort | hadron quark phase transition in the su 3 local nambu jona lasinio njl model with vector interaction |
| topic | quark matter NJL model RMF theory deconfinement phase transition Maxwell construction |
| url | https://www.mdpi.com/2073-8994/13/1/124 |
| work_keys_str_mv | AT grigoralaverdyan hadronquarkphasetransitioninthesu3localnambujonalasinionjlmodelwithvectorinteraction |