Parada T. P. Hutauruk, Hana Gil, Seung-il Nam, Chang Ho Hyun
{"title":"对称能对混合中子星状态方程的影响","authors":"Parada T. P. Hutauruk, Hana Gil, Seung-il Nam, Chang Ho Hyun","doi":"10.1007/s40042-024-01148-x","DOIUrl":null,"url":null,"abstract":"<div><p>In this study, we explore the impact of symmetry energy on the transitions between hadron and quark phases within compact stars. We investigate the properties of potential configurations of quark-hadron hybrid stars using energy-density functional (EDF) models and the flavor SU(2) Nambu–Jona-Lasinio (NJL) model, employing Schwinger’s covariant proper-time regularization scheme. In this theoretical framework, we utilize equations of state (EoSs) of hadronic matter obtained from EDF models to describe the hadronic phase, and the flavor SU(2) NJL model with varying repulsive-vector interaction strengths represents the quark phase. By solving the Tolman–Oppenheimer–Volkoff equation, we examine the mass-radius properties of the hybrid star configurations for different vector interactions and nuclear symmetry energies. Our findings show that the critical density at which the phase transition occurs ranges from 3.6 to 6.7 times the normal nuclear-matter density, depending on the symmetry energy and the strength of the vector coupling (<span>\\(G_v\\)</span>). The value of <span>\\(G_v\\)</span> influences the maximum mass of the neutron star (NS). In the absence of a repulsive force, the maximum mass of the NS is only about 1.5 times the mass of the Sun (<span>\\(M_\\odot\\)</span>). Still, it exceeds 2.0<span>\\(M_\\odot\\)</span> when the vector coupling constant is approximately half of the attractive scalar coupling constant. Interestingly, quark matter does not impact the canonical mass of NS (1.4<span>\\(M_\\odot\\)</span>). Therefore, observing the canonical mass of NSs can provide valuable constraints on the EoS of hadronic matter at high densities.</p></div>","PeriodicalId":677,"journal":{"name":"Journal of the Korean Physical Society","volume":"85 8","pages":"617 - 627"},"PeriodicalIF":0.8000,"publicationDate":"2024-07-25","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":"0","resultStr":"{\"title\":\"Effects of symmetry energy on the equation of state for hybrid neutron stars\",\"authors\":\"Parada T. P. Hutauruk, Hana Gil, Seung-il Nam, Chang Ho Hyun\",\"doi\":\"10.1007/s40042-024-01148-x\",\"DOIUrl\":null,\"url\":null,\"abstract\":\"<div><p>In this study, we explore the impact of symmetry energy on the transitions between hadron and quark phases within compact stars. We investigate the properties of potential configurations of quark-hadron hybrid stars using energy-density functional (EDF) models and the flavor SU(2) Nambu–Jona-Lasinio (NJL) model, employing Schwinger’s covariant proper-time regularization scheme. In this theoretical framework, we utilize equations of state (EoSs) of hadronic matter obtained from EDF models to describe the hadronic phase, and the flavor SU(2) NJL model with varying repulsive-vector interaction strengths represents the quark phase. By solving the Tolman–Oppenheimer–Volkoff equation, we examine the mass-radius properties of the hybrid star configurations for different vector interactions and nuclear symmetry energies. Our findings show that the critical density at which the phase transition occurs ranges from 3.6 to 6.7 times the normal nuclear-matter density, depending on the symmetry energy and the strength of the vector coupling (<span>\\\\(G_v\\\\)</span>). The value of <span>\\\\(G_v\\\\)</span> influences the maximum mass of the neutron star (NS). In the absence of a repulsive force, the maximum mass of the NS is only about 1.5 times the mass of the Sun (<span>\\\\(M_\\\\odot\\\\)</span>). Still, it exceeds 2.0<span>\\\\(M_\\\\odot\\\\)</span> when the vector coupling constant is approximately half of the attractive scalar coupling constant. Interestingly, quark matter does not impact the canonical mass of NS (1.4<span>\\\\(M_\\\\odot\\\\)</span>). Therefore, observing the canonical mass of NSs can provide valuable constraints on the EoS of hadronic matter at high densities.</p></div>\",\"PeriodicalId\":677,\"journal\":{\"name\":\"Journal of the Korean Physical Society\",\"volume\":\"85 8\",\"pages\":\"617 - 627\"},\"PeriodicalIF\":0.8000,\"publicationDate\":\"2024-07-25\",\"publicationTypes\":\"Journal Article\",\"fieldsOfStudy\":null,\"isOpenAccess\":false,\"openAccessPdf\":\"\",\"citationCount\":\"0\",\"resultStr\":null,\"platform\":\"Semanticscholar\",\"paperid\":null,\"PeriodicalName\":\"Journal of the Korean Physical Society\",\"FirstCategoryId\":\"101\",\"ListUrlMain\":\"https://link.springer.com/article/10.1007/s40042-024-01148-x\",\"RegionNum\":4,\"RegionCategory\":\"物理与天体物理\",\"ArticlePicture\":[],\"TitleCN\":null,\"AbstractTextCN\":null,\"PMCID\":null,\"EPubDate\":\"\",\"PubModel\":\"\",\"JCR\":\"Q3\",\"JCRName\":\"PHYSICS, MULTIDISCIPLINARY\",\"Score\":null,\"Total\":0}","platform":"Semanticscholar","paperid":null,"PeriodicalName":"Journal of the Korean Physical Society","FirstCategoryId":"101","ListUrlMain":"https://link.springer.com/article/10.1007/s40042-024-01148-x","RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":null,"EPubDate":"","PubModel":"","JCR":"Q3","JCRName":"PHYSICS, MULTIDISCIPLINARY","Score":null,"Total":0}
Effects of symmetry energy on the equation of state for hybrid neutron stars
In this study, we explore the impact of symmetry energy on the transitions between hadron and quark phases within compact stars. We investigate the properties of potential configurations of quark-hadron hybrid stars using energy-density functional (EDF) models and the flavor SU(2) Nambu–Jona-Lasinio (NJL) model, employing Schwinger’s covariant proper-time regularization scheme. In this theoretical framework, we utilize equations of state (EoSs) of hadronic matter obtained from EDF models to describe the hadronic phase, and the flavor SU(2) NJL model with varying repulsive-vector interaction strengths represents the quark phase. By solving the Tolman–Oppenheimer–Volkoff equation, we examine the mass-radius properties of the hybrid star configurations for different vector interactions and nuclear symmetry energies. Our findings show that the critical density at which the phase transition occurs ranges from 3.6 to 6.7 times the normal nuclear-matter density, depending on the symmetry energy and the strength of the vector coupling (\(G_v\)). The value of \(G_v\) influences the maximum mass of the neutron star (NS). In the absence of a repulsive force, the maximum mass of the NS is only about 1.5 times the mass of the Sun (\(M_\odot\)). Still, it exceeds 2.0\(M_\odot\) when the vector coupling constant is approximately half of the attractive scalar coupling constant. Interestingly, quark matter does not impact the canonical mass of NS (1.4\(M_\odot\)). Therefore, observing the canonical mass of NSs can provide valuable constraints on the EoS of hadronic matter at high densities.
期刊介绍:
The Journal of the Korean Physical Society (JKPS) covers all fields of physics spanning from statistical physics and condensed matter physics to particle physics. The manuscript to be published in JKPS is required to hold the originality, significance, and recent completeness. The journal is composed of Full paper, Letters, and Brief sections. In addition, featured articles with outstanding results are selected by the Editorial board and introduced in the online version. For emphasis on aspect of international journal, several world-distinguished researchers join the Editorial board. High quality of papers may be express-published when it is recommended or requested.