Phases of Hadron-Quark Matter in (Proto) Neutron Stars
In the first part of this paper, we investigate the possible existence of a structured hadron-quark mixed phase in the cores of neutron stars. This phase, referred to as the hadron-quark pasta phase, consists of spherical blob, rod, and slab rare phase geometries. Particular emphasis is given to mod...
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MDPI AG
2019-07-01
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| Series: | Universe |
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| Online Access: | https://www.mdpi.com/2218-1997/5/7/169 |
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| author | Fridolin Weber Delaney Farrell William M. Spinella Germán Malfatti Milva G. Orsaria Gustavo A. Contrera Ian Maloney |
| author_facet | Fridolin Weber Delaney Farrell William M. Spinella Germán Malfatti Milva G. Orsaria Gustavo A. Contrera Ian Maloney |
| author_sort | Fridolin Weber |
| collection | DOAJ |
| description | In the first part of this paper, we investigate the possible existence of a structured hadron-quark mixed phase in the cores of neutron stars. This phase, referred to as the hadron-quark pasta phase, consists of spherical blob, rod, and slab rare phase geometries. Particular emphasis is given to modeling the size of this phase in rotating neutron stars. We use the relativistic mean-field theory to model hadronic matter and the non-local three-flavor Nambu−Jona-Lasinio model to describe quark matter. Based on these models, the hadron-quark pasta phase exists only in very massive neutron stars, whose rotational frequencies are less than around 300 Hz. All other stars are not dense enough to trigger quark deconfinement in their cores. Part two of the paper deals with the quark-hadron composition of hot (proto) neutron star matter. To this end we use a local three-flavor Polyakov−Nambu−Jona-Lasinio model which includes the ’t Hooft (quark flavor mixing) term. It is found that this term leads to non-negligible changes in the particle composition of (proto) neutron stars made of hadron-quark matter. |
| first_indexed | 2024-04-14T06:48:49Z |
| format | Article |
| id | doaj.art-b9fee90b48c14604b60de5ed905b1c4e |
| institution | Directory Open Access Journal |
| issn | 2218-1997 |
| language | English |
| last_indexed | 2024-04-14T06:48:49Z |
| publishDate | 2019-07-01 |
| publisher | MDPI AG |
| record_format | Article |
| series | Universe |
| spelling | doaj.art-b9fee90b48c14604b60de5ed905b1c4e2022-12-22T02:07:06ZengMDPI AGUniverse2218-19972019-07-015716910.3390/universe5070169universe5070169Phases of Hadron-Quark Matter in (Proto) Neutron StarsFridolin Weber0Delaney Farrell1William M. Spinella2Germán Malfatti3Milva G. Orsaria4Gustavo A. Contrera5Ian Maloney6Department of Physics, San Diego State University, San Diego, CA 92182, USADepartment of Physics, San Diego State University, San Diego, CA 92182, USADepartment of Sciences, Wentworth Institute of Technology, 550 Huntington Avenue, Boston, MA 02115, USAGrupo de Gravitación, Astrofísica y Cosmología, Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional de La Plata, Paseo del Bosque S/N, La Plata 1900, ArgentinaGrupo de Gravitación, Astrofísica y Cosmología, Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional de La Plata, Paseo del Bosque S/N, La Plata 1900, ArgentinaGrupo de Gravitación, Astrofísica y Cosmología, Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional de La Plata, Paseo del Bosque S/N, La Plata 1900, ArgentinaDepartment of Physics, San Diego State University, San Diego, CA 92182, USAIn the first part of this paper, we investigate the possible existence of a structured hadron-quark mixed phase in the cores of neutron stars. This phase, referred to as the hadron-quark pasta phase, consists of spherical blob, rod, and slab rare phase geometries. Particular emphasis is given to modeling the size of this phase in rotating neutron stars. We use the relativistic mean-field theory to model hadronic matter and the non-local three-flavor Nambu−Jona-Lasinio model to describe quark matter. Based on these models, the hadron-quark pasta phase exists only in very massive neutron stars, whose rotational frequencies are less than around 300 Hz. All other stars are not dense enough to trigger quark deconfinement in their cores. Part two of the paper deals with the quark-hadron composition of hot (proto) neutron star matter. To this end we use a local three-flavor Polyakov−Nambu−Jona-Lasinio model which includes the ’t Hooft (quark flavor mixing) term. It is found that this term leads to non-negligible changes in the particle composition of (proto) neutron stars made of hadron-quark matter.https://www.mdpi.com/2218-1997/5/7/169quark matterhadronic matterquark deconfinementneutron star matternuclear equation of statephase transition |
| spellingShingle | Fridolin Weber Delaney Farrell William M. Spinella Germán Malfatti Milva G. Orsaria Gustavo A. Contrera Ian Maloney Phases of Hadron-Quark Matter in (Proto) Neutron Stars Universe quark matter hadronic matter quark deconfinement neutron star matter nuclear equation of state phase transition |
| title | Phases of Hadron-Quark Matter in (Proto) Neutron Stars |
| title_full | Phases of Hadron-Quark Matter in (Proto) Neutron Stars |
| title_fullStr | Phases of Hadron-Quark Matter in (Proto) Neutron Stars |
| title_full_unstemmed | Phases of Hadron-Quark Matter in (Proto) Neutron Stars |
| title_short | Phases of Hadron-Quark Matter in (Proto) Neutron Stars |
| title_sort | phases of hadron quark matter in proto neutron stars |
| topic | quark matter hadronic matter quark deconfinement neutron star matter nuclear equation of state phase transition |
| url | https://www.mdpi.com/2218-1997/5/7/169 |
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